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Home , Beta Aurigae, EF Eridani, EX Hydrae, GD 362, SU Ursae Majoris, Symbiotic binary

Interacting Binaries No. 28, May 1st, 2007 An Electronic Newsletter Editors: Boris T. Gansicke¨ Dept. of Physics, University of Warwick, Coventry CV4 7AL, UK Andrew J. Norton Dept. of Physics & Astronomy, The Open University, Milton Keynes MK7 6AA, UK

[email protected], http://astrocat.org/ibnews Contents

1 Editorial 2

2 Abstracts of refereed papers 3 – HS1857+5144: A hot and young pre-cataclysmic variable Aungwerojwit et al...... 3 – Analysis of the first confirmed superoutburst of V337 Cygni in 2006 May Boyd et al...... 3 – Spitzer Space Telescope observations of magnetic cataclysmic variables: possibilities for the presence of dust in polars Brinkworth et al ...... 4 – ULTRACAM: an ultra-fast, triple-beam CCD camera for high-speed astrophysics Dhillon et al .... 4 – On the abundances of GRO J1655-40 Foellmi, Dall & Depagne ...... 5 – Evolution of Close Binaries Gokhale, Xiao & Frank ...... 5 – SDSS J102146.44+234926.3:New WZ Sge-type dwarf Golovin et al...... 6 – Cool companions to white dwarf from the Two Micron All Sky Survey All Sky Data Re- lease Hoard et al ...... 6 – Formation of relativistic jets by collapsing stars to black holes Kryvdyk ...... 7 – A Synthetic Spectrum and Light Curve Analysis of the Cataclysmic Variable IX Velorum Linnell et al. 7 – IGR J16194−2810: a new symbiotic X–ray binary Masetti et al...... 8 – Hydrodynamic and Spectral Simulations of HMXB Winds Mauche et al ...... 8 – Astrophysics of white dwarf binaries Nelemans ...... 8 – New periodic variable stars coincident with ROSAT sources discovered using SuperWASP Norton et al 9 – Long-term monitoring of the short period SU UMa-type , V844 Herculis Oizumi et al. ... 10 – Emission Line Flickering from the Secondary in Cataclysmic Variables? A study of V3885 Sagi- tarii Ribeiro & Diaz ...... 10 – SW Sextantis stars: the dominant population of CVs with orbital periods between 3–4hours Rod´ıguez- Gil et al...... 11 – XMM-Newtonobservationsof EF Eridani: the textbookexample of low- rate polars Schwope et al ...... 12 – Equipotential Surfaces and Lagrangian Points in Non-synchronous, Eccentric Binary and Planetary Systems Sepinsky, Willems & Kalogera ...... 12 – Spectroscopy of Nine Cataclysmic Variable Stars Sheets et al ...... 13 – On the effect of emission lines on the UBVR Skopal ...... 13 – Comprehensive simulations of Smith et al...... 14 – SDSSJ233325.92+152222.1 and the evolution of intermediate polars Southworth et al ...... 14 – Cataclysmic Variables from SDSS VI. The Sixth (2005) Szkody et al ...... 15 – On the of the magnetic Cataclysmic Variable HS 0922+1333 Tovmassian & Zharikov .. 15

3 Abstracts of theses 16 – Mass Transfer and Evolution of Compact Binary Stars Gokhale ...... 16 1 EDITORIAL 2

4 As seen onastro-ph 16 4.1 CataclysmicVariablesandrelatedsystems ...... 16 4.2 LMXBsandrelatedsystems ...... 19 4.3 HMXBsandrelatedsystems ...... 22 4.4 ULXsandextragalacticXRBs ...... 24 4.5 Accretiondiscsandaccretiontheory ...... 24 4.6 Mergers,SNIa,andaccretioninducedcollapse...... 25 4.7 Radiopulsarsinbinaries(andotherwise)...... 25 4.8 :AXPsandSGRs ...... 26 4.9 Otherbinarysystems ...... 27

1 Editorial

Dear IB friends,

Welcome to this edition of the Interacting Binaries Newsletter. Like the last one, this edition appears only 3 months after the previous edition so hopefully the abstracts of the papers listed here are still fresh. It’s also nice to see some new contributors to the newsletter – we hope you continue to find this to be a useful resource. As always, we’re on the look out for as many articles as possible in each issue, so if any of your colleagues are not in the habit of sending in abstracts, please encourage them to do so for the next edition, which will be in another 3 months or so. The astro-ph listing in this edition would normally have been quite short, but owing to a production error last time, we include here 6 months’ worth of abstracts for your perusal – see that section of this newsletter for details! As always: happy reading, Boris Gansicke¨ & Andy Norton

Download/Website: http://www.warwick.ac.uk/staff/Boris.Gaensicke/IBNews/ Contact: [email protected] 2 ABSTRACTS OF REFEREED PAPERS 3

2 Abstracts of refereed papers HS1857+5144: A hot and young pre-cataclysmic variable A. Aungwerojwit1,2,B.T.Gansicke¨ 1, P.Rodr´ıguez-Gil3, H.-J. Hagen4, O. Giannakis5, C. Papadimitriou5, C. Allende Prieto6, D. Engels4 1 Department of Physics, University of Warwick, Coventry, CV4 7AL, UK 2 Department of Physics, Faculty of Science, Naresuan University, Phitsanulok, 65000, Thailand 3 Instituto de Astrof´ısica de Canarias, 38200 La Laguna, Tenerife, Spain 4 Hamburger Sternwarte, Universit¨at Hamburg, Gojenbergsweg 112, 21029 Hamburg, Germany 5 Institute of Astronomy and Astrophysics, National Observatory of Athens, P.O. Box 20048, Athens 11810, Greece 6 McDonald Observatory and Department of Astronomy, University of Texas, Austin, TX 78712, USA Astronomy & Astrophysics, in press (arXiv:0704.1780)

We report the discovery of a new white dwarf/M dwarf binary, HS1857+5144, identified in the Hamburg Quasar Survey (HQS). Time-resolved optical spectroscopy and photometry were carried out to determine the properties of this new cataclysmic variable progenitor (pre-CV). The light curves of HS1857+5144 display a sinusoidal variation with a period of Porb = 383.52min and peak-to-peak amplitudes of 0.7mag and 1.1mag in the B-band and R-band, respectively. The large amplitude of the brightness variation results from a reflection effect on the heated inner hemisphere of the companion star, suggesting a very high temperature of the white dwarf. Our study confirms the photometric period as the orbital period of the system. A model atmosphere fit to the spectrum of the white dwarf obtained at minimum light provides limits to its mass and temperature of Mwd ≃ 0.6 − 1.0M⊙ and Twd ≃ 70000 − 100000K, respectively. The detection of HeII λ 4686 absorption classifies the primary star of HS1857+5144as a DAO white dwarf. Combiningthe results from our spectroscopy and photometry,we estimate the ◦ ◦ mass of the companion star and the binary inclination to be Msec ≃ 0.15 − 0.30 M⊙ and i ≃ 45 − 55 , respectively. We classify HS1857+5144 as one of the youngest pre-CV known to date. The cooling age of the white dwarf suggests that the present system has just emerged from a phase ∼ 105 yr ago. HS1857+5144will start mass transfer within or below the 2–3h period gap. Download/Website: http://uk.arxiv.org/abs/0704.1780 Contact: [email protected]

Analysis of the first confirmed superoutburst of V337 Cygni in 2006 May D. Boyd1, T. Krajci2, J. Shears3, G. Poyner4 1 5 Silver Lane, West Challow, Wantage, Oxon, OX12 9TX, UK 2 PO Box 1351 Cloudcroft, New Mexico 88317, USA 3 ”Pemberton”, School Lane, Bunbury, Tarporley, Cheshire, CW6 9NR, UK 4 67 Ellerton Road, Kingstanding, Birmingham, B44 0QE, UK Journal of the British Astronomical Association, in press (astro-ph/0702607),

During 2006 May the first confirmed superoutburst of the dwarf nova V337 Cygni was observed using unfiltered CCD photometry. The outburst reached a peak of 15.2 on May 22 and lasted 13 days before the ob- ject returned to quiescence at around magnitude 20. Time-series photometry revealed superhumps with a period of 0.07012 +/- 0.00033d and amplitude 0.1 magnitude, thereby establishing for the first time its UGSU classifica- tion. of V337 Cyg in outburst determined an accurate position and enabled the identity of the star in quiescence to be confirmed. Download/Website: http://arxiv.org/abs/astro-ph/0702607 Contact: [email protected] 2 ABSTRACTS OF REFEREED PAPERS 4

Spitzer Space Telescope observations of magnetic cataclysmic variables: possibilities for the presence of dust in polars C. S. Brinkworth1, D. W. Hoard1, S. Wachter1, S. B. Howell2, David R. Ciardi3, P. Szkody4, T. E. Harrison5, G. T. van Belle3, A. A. Esin6 1 Spitzer Science Center, California Institute of Technology, Pasadena, CA 91125, USA 2 WIYN Observatory/National Optical Astronomy Observatory, Tucson, AZ 85719, USA 3 Michelson Science Center, California Institute of Technology, Pasadena, CA 91125, USA 4 Department of Astronomy, University of Washington, Seattle, WA 98195-1580, USA 5 Department of Astronomy, New Mexico State University, Las Cruces, NM 88003, USA 6 Department of Physics, Harvey Mudd College, Claremont, CA 91711-5990, USA The Astrophysical Journal, published (2007ApJ...659.1541B)

We present Spitzer Space Telescope photometry of six short-period polars, EF Eri, V347 Pav, VV Pup, V834 Cen, GG Leo, and MR Ser. We have combined the Spitzer Array Camera (3.6–8.0 µm) data with the 2MASS JHKs photometry to construct the spectral energy distributions of these systems from the near- to mid-IR (1.235–8 µm). We find that five out of the six polars have flux densities in the mid-IR that are substantially in excess of the values expected from the stellar components alone. We have modeled the observed SEDs with a combination of contributions from the white dwarf, secondary star, and either cyclotron emission or a cool, circumbinary dust disk to fill in the long-wavelength excess. We find that a circumbinary dust disk is the most likely cause of the 8µm excess in all cases, but we have been unable to rule out the specific (but unlikely) case of completely optically thin cyclotron emission as the source of the observed 8µm flux density. While both model components can generate enough flux at 8µm, neither dust nor cyclotron emission alone can match the excess above the stellar components at all wavelengths. A model combining both cyclotron and dust contributions, possibly with some accretion-generated flux in the near-IR, is probablyrequired, but our observed SEDs are not sufficiently well-sampled to constrain such a complicated model. If the 8 µm flux density is caused by the presenceof a circumbinarydust disk, then our estimates of the masses of these disks are many orders of magnitude below the mass required to affect CV evolution. Contact: [email protected]

ULTRACAM: an ultra-fast, triple-beam CCD camera for high-speed astrophysics V. S. Dhillon1, T. R. Marsh2, M. J. Stevenson1, D. C. Atkinson3, P. Kerry1, P. T. Peacocke3, A. J. A. Vick3, S. M. Beard3, D. J. Ives3, D. W. Lunney3, S. A. McLay3, C. J. Tierney3, J. Kelly1, S. P. Littlefair1, R. Nicholson1, R. Pashley1, E. T. Harlaftis4, K. O’Brien5 1 Department of Physics and Astronomy, University of Sheffield, Sheffield S3 7RH, UK 2 Department of Physics, University of Warwick, Coventry CV4 7AL, UK 3 UK Astronomy Technology Centre, Royal Observatory Edinburgh, Blackford Hill, Edinburgh EH9 3HJ, UK 4 Institute of Space Applications and Remote Sensing, National Observatory of Athens, Lofos Koufou, Palaia Penteli, Athens 152 36, Greece 5 European Southern Observatory, Alonso de Cordova 3107, Vitacura, Casilla 1 9001, Santiago 19, Chile Monthly Notices of the Royal Astronomical Society, in press, astro-ph/0704.2557

ULTRACAM is a portable, high-speed imaging photometer designed to study faint astronomical objects at high temporal resolutions. ULTRACAM employs two dichroic beamsplitters and three frame-transfer CCD cameras to provide three-colour optical imaging at frame rates of up to 500 Hz. The instrument has been mounted on both the 4.2-m William Herschel Telescope on La Palma and the 8.2-m Very Large Telescope in Chile, and has been used to study white dwarfs, brown dwarfs, , black-hole/neutron-star X-ray binaries, gamma-ray bursts, cata- clysmic variables, eclipsing binary stars, extrasolar , flare stars, ultra-compact binaries, active galactic nuclei, and occultations by objects (Titan, Pluto and Kuiper Belt objects). In this paper we describe the scientific motivation behind ULTRACAM, present an outline of its design and report on its measured performance. 2 ABSTRACTS OF REFEREED PAPERS 5

Download/Website: http://xxx.soton.ac.uk/abs/0704.2557 Contact: [email protected]

On the abundances of GRO J1655-40 C. Foellmi1,2, T.H. Dall3, E. Depagne1,4 1 European Southern Observatory, 3107 Alonso de Cordova, Casilla 19001, Vitacura, Santiago, Chile 2 Laboratoire d’Astrophysique, Observatoire de Grenoble, BP 53, 38041 Grenoble Cedex 9, France 3 Gemini Observatory, 670 N. A’ohoku Place, Hilo, HI 96720, USA 4 Departamento de Astronom´ıa y Astrof´ısica, Pontificia Universidad Cat´olica de Chile, Campus San Joaqu´ın. Vicu˜na Mackenna 4860 Casilla 306, Santiago 22, Chile. Astronomy and Astrophysics, published (2007A&A...464L..61F)

The detection of overabundances of α-elements and lithium in the secondary star of a black-hole binary provides important insights about the formation of a stellar-mass black-hole. α- enhancement might theoretically also be the result of pollution by the nucleosynthesis occurring during an outburst, or through spallation by the jet. We study the abundances, and their possible variations with time, in the secondary star of the runaway black-hole binary GRO J1655–40, in order to understand their origin. We present a detailed comparison between a Keck spectrum obtained in 1998 found in the literature, archival VLT- UVES data taken in 2004 and new VLT-UVES spectra obtained early 2006. We carefully determine the equivalent widths of different α-elements (Mg, O, Ti, S and Si) with their associated uncertainty. We use the well-studied comparison star HD 156098 as well as synthetic spectra to match the spectrum of GRO J1655–40 in order to determine the abundances of these elements. We see no significant variations of equivalent widths with time. Our fit using HD 156098 reveals that there is significant overabundance of oxygen in all our spectra, but no overabundances of any of the other α-elements. Finally, we do not detect the lithium line at 6707 A.˚ We show that there is no detected pollution in GRO J1655–40 after the burst in 2005. Moreover, we argue that uncertainties in the equivalent widths were previously underestimated by a factor of ∼3. Consequently, our results challenge the existence of general overabundances of α-elements observed in this galactic black- hole binary, and thus the accepted interpretation that they are of origin. The physical cause of the overabundanceof oxygen remains unclear. Contact: [email protected]

Evolution of Close White Dwarf Binaries Vayujeet Gokhale, Xiao Meng Peng, Juhan Frank Department of Physics & Astronomy, Louisiana State University, Baton Rouge, LA 70803-4001 The Astrophysical Journal, published (2007ApJ...655.1010G/astro-ph/0610919)

We describe the evolution of double degenerate binary systems, consisting of components obeying the zero- temperature mass-radius relationship for white dwarf stars, from the onset of mass transfer to one of several possible outcomes, including merger, tidal disruption of the donor, or survival as a semidetached AM CVn system. We use a combination of analytic solutions and numerical integrations of the standard -averaged first-order evolution equations, including direct-impact accretion and the evolution of the components due to mass exchange. We in- clude also the effects of mass loss during supercritical (super-Eddington) mass transfer and the tidal and advective exchanges of angular momentum between the binary components. With the caveat that our formalism does not in- clude an explicit treatment of common-envelopephases, our results suggest that a larger fraction of detached double white dwarfs survive the onset of mass transfer than has been hitherto assumed, even if this mass transfer is initially 2 ABSTRACTS OF REFEREED PAPERS 6 unstable and rises to super-Eddington levels. In addition, as a consequence of the tidal coupling, systems that come into contact near the mass transfer instability boundary undergo a phase of oscillation cycles in their orbital period (and other system parameters). Unless the donor star has a finite entropy such that the effective mass-radius relation- ship deviates significantly from that of a zero-temperature white dwarf, we expect our results to be valid. Much of the formalism developed here would also apply to other mass-transferring binaries, and in particular to cataclysmic variables and Algol systems. Contact: [email protected]

SDSS J102146.44+234926.3: New WZ Sge-type dwarf nova Golovin, Alex1,2,3; Ayani, Kazuya4; Pavlenko, Elena P.5; Krajci, Tom6; Kuznyetsova, Yuliana2,7; Henden, Arne8; Krushevska, Victoria2; Dvorak, Shawn9; Sokolovsky, Kirill10,11; Sergeeva, Tatyana P.2; James, Robert12; Crawford, Tim13; Corp, Laurent14; 1 Kyiv National Taras Shevchenko University, Kyiv, UKRAINE 2 Main Astronomical Observatory of National Academy of Science of Ukraine, Kyiv, UKRAINE 3 Visiting astronomer of the Crimean Astrophysical Observatory, Crimea, Nauchnyj, UKRAINE 4 Bisei Astronomical Observatory, Ibara, Okayama, JAPAN 5 Crimean Astrophysical Observatory, Crimea, Nauchnyj, UKRAINE 6 AAVSO, Cloudcroft, New Mexico, USA 7 International Center of Astronomical and Medico-Ecological Researches, Kyiv, UKRAINE 8 AAVSO, Clinton B. Ford Astronomical Data and Research Center, Cambridge, MA, USA 9 Rolling Hills Observatory, Clermont, FL, USA 10 Sternberg Astronomical Institute, Moscow State University, Moscow, RUSSIA 11 Astro Space Center of the Lebedev Physical Institute, Russian Academy of Sciences, Moscow, RUSSIA 12 AAVSO, Las Cruses, NM, USA 13 AAVSO, Arch Cape Observatory, Arch Cape, OR, USA 14 AAVSO, Rodez, FRANCE IBVS 5763, published (2007IBVS.5763....1G/arXiv:0704.1276)

We report CCD photometry and spectroscopy during 2006 outburst of the dwarf nova SDSS J102146.44+234926.3 (SDSS J1021). The photographic plates from the MAO, SAI and CrAO plate archives, which cover the position of the SDSS J1021, were inspected for the presence of previous outbursts. We also present the BVRcIc photometric calibration of 52 stars in SDSS J1021 vicinity, which have V-magnitudein the range of 11.m21-17.m23 and can serve as comparison stars. The large amplitude of the SDSS J1021 outburst of 7m, superhumps with a period below the ”period gap”, rebrightening during the declining stage of superoutburst, rarity of outbursts and obtained spectrum allow to classify this object as a WZ Sge type dwarf nova. Contact: [email protected], astronom [email protected]

Cool companions to white dwarf stars from the Two Micron All Sky Survey All Sky Data Release D. W. Hoard1, S. Wachter1, Laura K. Sturch1,2, Allison M. Widhalm1,3,4, Kevin P. Weiler1,5,6, Magaretha L. Pretorius1,7, Joseph W. Wellhouse1,2,4, Maxsim Gibiansky1,2 1 Spitzer Science Center, California Institute of Technology, Pasadena, CA 91125, USA 2 Department of Physics, Harvey Mudd College, Claremont, CA 91711-5990, USA 3 Department of Physics and Astronomy, University of Southern California, Los Angeles, CA 90089, USA 4 Department of Astronomy, New Mexico State University, Las Cruces NM 88003-8001, USA 5 Department of Physics, Marquette University, Milwaukee, WI 53201, USA 6 Department of Physics, DePaul University, Chicago IL 60614, USA 7 School of Physics & Astronomy, University of Southampton, Southampton, SO17 1BJ, United Kingdom The Astronomical Journal, in press (astro-ph/0702754) 2 ABSTRACTS OF REFEREED PAPERS 7

We present the culmination of our near-infrared survey of the optically spectroscopically identified white dwarf stars from the McCook & Sion catalog, conducted using photometric data from the Two Micron All Sky Survey final All Sky Data Release. The color-selection technique, which identifies candidate binaries containing a white dwarf and a low mass stellar (or sub-stellar) companion via their distinctive locus in the near-infrared color-color diagram, is demonstrated to be simple to apply and to yield candidates with a high rate of subsequent confirmation. We recover 105 confirmed binaries, and identify 27 firm candidates (19 of which are new to this work) and 21 tentative candidates (17 of which are new to this work) from the 2MASS data. Only a small number of candidates from our survey have likely companion spectral types later than M5, none of which is an obvious L type (i.e., potential ) companion. Only one previously known WD + brown dwarf binary is detected. This result is discussed in the context of the 2MASS detection limits, as well as other recent observational surveys that suggest a very low rate of formation (or survival) for binary stars with extreme mass ratios. Download/Website: http://spider.ipac.caltech.edu/staff/hoard/research/wdir/index.html Contact: [email protected]

Formation of relativistic jets by collapsing stars to black holes V.Kryvdyk National Taras Shevchenko University of Kyiv, Faculty of Physics, av. Glushkova 2, Kyiv, Ukraine Adv. Space Res., in press Formation of relativistic jets in the magnetosphere of collapsing stars is considered. These jets will be formed in the caps of magnetosphere of collapsing star, where the stellar magnetic field increases during the collapse and the charged particles are accelerated. The jets will generate non-thermal radiation. The analysis of dynamics and emission of particles in the stellar magnetosphere under collapse shows that collapsing stars can by powerful sources of relativistic jets. Contact: [email protected]

A Synthetic Spectrum and Light Curve Analysis of the Cataclysmic Variable IX Velorum Albert P. Linnell1, Patrick Godon2, Ivan Hubeny3, Edward M. Sion4, Paula Szkody1 1 Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195-1580 2 Department of Astronomy and Astrophysics, Villanova University, Villanova, PA 19085 visiting at the Space Telescope Institute, Baltimore, MD. 3 Steward Observatory and Department of Astronomy, University of Arizona, Tucson, AZ 85721 4 Department of Astronomy and Astrophysics, Villanova University, Villanova, PA 19085 Astrophysical Journal, [refereed journal] in press Spectrum synthesis analysis of FUSE and STIS spectra for the cataclysmic variable IX Vel shows that it is possible −9 −1 to achieve a close synthetic spectrum fit with a mass transfer rate of M˙ = 5×10 M⊙/yr and a modified stan- dard model temperature profile. The innermost four annuli of the model, extending to r/rwd≈4, are isothermal; beyond that limit the temperatures follow the standard model. A light synthesis fit to K band photometry requires shallow of the accretion disk rim and secondary star limb. The geometry constrains the to i = 57±2 ◦. The synthetic light curve requires a vertically extended accretion disk rim, beyond that predicted by gravitational equilibrium, to shadow the secondary star. The enhanced vertical extension is consistent with recent MHD predictions for CV accretion disks. Matching differing observed heights of alternate K band light curve maxima requires a warm rim region downstream of the intersection point of the mass transfer stream with the accretion disk rim. The temperature of the warm region is inconsistent with expectation for a bright spot associated with a rim shock. Contact: [email protected] 2 ABSTRACTS OF REFEREED PAPERS 8

IGR J16194−2810: a new symbiotic X–ray binary N. Masetti1, R. Landi1, M.L. Pretorius2, V. Sguera2, A.J. Bird2, M. Perri3, P.A. Charles4, J.A. Kennea5, A. Malizia1 and P. Ubertini6 1 INAF - Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna, via Gobetti 101, I-40129 Bologna, Italy 2 School of Physics & Astronomy, University of Southampton, Southampton, Hampshire, SO17 1BJ, United Kingdom 3 ASI Science Data Center, via Galileo Galilei, I-00044 Frascati, Italy 4 South African Astronomical Observatory, P.O. Box 9, Observatory 7935, South Africa 5 Pennsylvania State University, 525 Davey Laboratory, University Park, PA 16802, USA 6 INAF - Istituto di Astrofisica Spaziale e Fisica Cosmica di Roma, via Fosso del Cavaliere 100, I-00133 Roma, Italy Astronomy & Astrophysics, in press (arxiv:0704.3682[astro-ph])

We here report on the multiwavelength study which led us to the identification of X–ray source IGR J16194−2810 as a new Symbiotic X–ray Binary (SyXB), that is, a rare type of Low Mass X–ray Binary (LMXB) composed of a M-type giant and a compact object. Using the accurate X–ray position allowed by Swift/XRT data, we pin- pointed the optical counterpart, a M2III star. Besides, the combined use of the spectral information afforded by XRT and INTEGRAL/IBIS shows that the 0.5–200 keV spectrum of this source can be described with an absorbed Comptonization model, usually found in LMXBs and, in particular, in SyXBs. No long-term (days to months) pe- riodicities are detected in the IBIS data. The time coverage afforded by XRT reveals shot-noise variability typical of accreting Galactic X–ray sources, but is not good enough to explore the presence of X–ray short-term (seconds to ) oscillations in detail. By using the above information, we infer important parameters for this source such as its distance (∼3.7 kpc) and X–ray (∼1.4×1035 erg s−1 in the 0.5–200 keV band), and we give a description for this system (typical of SyXBs) in which a compact object (possibly a ) accretes from the wind of its M-type giant companion. We also draw some comparisons between IGR J16194−2810 and other sources belonging to this subclass, finding that this object resembles SyXBs 4U 1700+24 and 4U 1954+31. Download/Website: http://arxiv.org/abs/0704.3682 Contact: [email protected]

Hydrodynamic and Spectral Simulations of HMXB Winds Christopher W. Mauche1, Duane A. Liedahl1, Shizuka Akiyama1, Tomasz Plewa2 1 Lawrence Livermore National Laboratory, L-473, 7000 East Avenue, Livermore, CA 94550, USA 2 University of Chicago, 5640 S. Ellis Avenue, Chicago, IL 60637, USA Progress of Theoretical Physics, Supplement, in press (arxiv:0704.0237v1)

We describe preliminary results of a global model of the radiatively-driven photoionized wind and accretion flow of the high-mass X-ray binary Vela X-1. The full model combines FLASH hydrodynamic calculations, XSTAR photoionization calculations, HULLAC atomic data, and Monte Carlo radiation transport. We present maps of the density, temperature, velocity, and ionization parameter from a FLASH two-dimensional time-dependent simulation of Vela X-1, as well as maps of the emissivity distributions of the X-ray emission lines. Download/Website: http://arxiv.org/abs/0704.0237v1 Contact: [email protected]

Astrophysics of white dwarf binaries G. Nelemans Department of Astrophysics, IMAPP, Radboud University Nijmegen, The Netherlands Proceedings 6th LISA symposyum, published (astro-ph/0703292) 2 ABSTRACTS OF REFEREED PAPERS 9

White dwarf binaries are the most common compact binaries in the Universe and are especially important for low- frequency gravitational wave detectors such as LISA. There are a number of open questions about binary evolution and the Galactic population of white dwarf binaries that can be solved using gravitational wave data and at the same time, our ever improving knowledge about these binaries will help to predict the signals that can be expected for LISA. In addition a number of white dwarf binaries will serve as verification sources for the instrument. I will discuss these issues and report recent, surprising, developments in this field. Finally I report calculations about the feasibility of complementary electro-magnetic observations which unfortunately cannot reproduce the optimistic results of Cooray et al. (2004) Contact: [email protected]

New periodic variable stars coincident with ROSAT sources discovered using SuperWASP A.J. Norton1, P.J. Wheatley2, R.G. West3, C.A. Haswell1, R.A. Street4, A. Collier Cameron5, D.J. Christian4, W.I. Clarkson6, B. Enoch1, M. Gallaway1, C. Hellier7, K. Horne5, J. Irwin8, S.R. Kane9, T.A. Lister7, J.P. Nicholas2, N. Parley10, D. Pollacco4, R. Ryans4, I. Skillen11, D.M. Wilson7 1 Department of Physics and Astronomy, The Open University, Walton Hall, Milton Keynes MK7 6AA, U.K. 2 Department of Physics, University of Warwick, Coventry CV4 7AL, U.K. 3 Department of Physics and Astronomy, University of Leicester, Leicester LE1 7RH, U.K. 4 Astrophysics Research Centre, Main Physics Building, School of Mathematics & Physics, Queen’s University, University Road, Belfast BT7 1NN, U.K. 5 School of Physics and Astronomy, University of St. Andrews, North Haugh, St. Andrews, Fife KY16 9SS, U.K. 6 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, U.S.A. 7 Astrophysics Group, School of Chemistry & Physics, Keele University, Staffordshire ST5 5BG, U.K. 8 Institute of Astronomy, University of Cambridge, Madingly Road, Cambridge CB3 0HA, U.K. 9 Department of Physics, University of Florida, Gainesville, FL 32611-8440, U.S.A. 10 Planetary & Space Sciences Research Institute, The Open University, Walton Hall, Milton Keynes MK7 6AA, U.K. 11 Isaac Newton Group of Telescopes, Apartado de Correos 321, E-38700 Santa Cruz de la Palma, Tenerife, Spain Astronomy & Astrophysics, in press (astro-ph/0702631)

We present optical lightcurves of 428 periodic variable stars coincident with ROSAT X-ray sources, detected using the first run of the SuperWASP photometric survey. Only 68 of these were previously recognised as periodic vari- ables. A further 30 of these objects are previously known pre- stars, for which we detect a modulation period for the first time. Amongst the newly identified periodic variables, many appear to be close eclipsing bina- ries, their X-ray emission is presumably the result of RS CVn type behaviour. Others are probably BY Dra stars, pre-main sequence stars and other rapid rotators displaying enhanced coronal activity. A number of previously cat- alogued pulsating variables (RR Lyr stars and Cepheids) coincident with X-ray sources are also seen, but we show that these are likely to be misclassifications. We identify four objects which are probable low mass eclipsing binary stars, based on their very red colour and light curve morphology. Download/Website: http://physics.open.ac.uk/ ajnorton/wasp rosat Contact: [email protected] 2 ABSTRACTS OF REFEREED PAPERS 10

Long-term monitoring of the short period SU UMa-type dwarf nova, V844 Herculis S. Oizumi1, T. Omodaka1, H. Yamamoto1, S. Tanada1, T. Yasuda1, Y. Arao1, K. Kodama1, M. Suzuki1, T. Matsuo1, H. Maehara2, N. Nakajima3, P. A. Dubovsky4, T. Kato5, A. Imada5, K. Kubota5, K. Sugiyasu5, K. Morikawa6, K. Torii7, M. Uemura8, R. Ishioka9, K. Tanabe10, D. Nogami11 1 Faculty of Science, Kagoshima University,1-21-30 Korimoto, Kagoshima, Japan 2 VSOLJ, Namiki 1-13-4,Kawaguchi, Saitama, Japan 3 VSOLJ, 124 Isatotyo, Teradani, Kumano, Mie, Japan 4 Slovak Association of Amateur Astronomers, Podbiel, Slovakia 5 Department of Astronomy, Faculty of Science, Kyoto University, Sakyo-ku, Kyoto, Japan 6 468-3 Satoyamada, Yakage-cho, Oda-gun, Okayama, Japan 7 Department of and Space Science, Graduate School of Science, Osaka University, 1-1 Machikaneyama-cho, Toyonaka, Osaka, Japan 8 Hiroshima Astrophysical Science Center, Hiroshima University, Higashi-Hiroshima, Hiroshima, Japan 9 Subaru Telescope, National Astronomical Observatory of Japan, 650 North A’ohoku Place, Hilo, HI 96720, USA 10 Department of Biosphere-Geosphere Systems, Faculty of Informatics, Okayama University of Science, 1-1 Ridai-cho, Okayama, Okayama 11 Hida Observatory, Kyoto University, Kamitakara, Gifu, Japan Publications of the Astronomical Society of Japan, in press (astro-ph/0702752)

We report on time-resolved CCD photometry of four outbursts of a short-period SU UMa-type dwarf nova, V844 Herculis. We successfully determined the mean periods to be 0.05584(64) days, and 0.055883(3) for the 2002 May superoutburst, and the 2006 April-May superoutburst, respectively. During the 2002 October obser- vations, we confirmed that the outburst is a normal outburst, which is the first recorded normal outburst in V844 Her. We also examined superhump period changes during 2002 May and 2006 April-May superoutbursts, both of which showed increasing superhump period over the course of the plateau stage. In order to examine the long-term behavior of V844 Her, we analyzed archival data over the past ten since the discovery of this binary. Al- though photometry is not satisfactory in some superoutbursts, we found that V844 Her showed no precursors and rebrightenings. Based on the long-term light curve, we further confirmed V844 Her has shown almost no n ormal outbursts despite the fact that the supercycle of the system is estimated to be about 300 days. In order to explain the long-term light curves of V844 Her, evaporation in the accretion disk may play a role in the avoidance of several normal outbursts, which does not contradict with the relatively large X-ray luminosity of V844 Her. Contact: a [email protected]

Emission Line Flickering from the Secondary Star in Cataclysmic Variables? A study of V3885 Sagitarii Ribeiro, Fabiola M. A.; Diaz, Marcos P. Universidade de Sa˝ao Paulo, Brazil The Astronomical Journal, in press (astro-ph/0702308)

Spectrophotometric observations of H-alpha and He I 6678 emission lines of the nova-like Cataclysmic Variable V3885 Sgr are presented and analyzed. The binary orbital period was determined as P = 0.20716071(22) days. Doppler Tomography was performed with both H-alpha and He I lines. Disc radial emissivity profiles were also computed. The tomography mapping of flickering sources was performed using the H-alpha line, from which we concluded that the flickering is not uniformly distributed on the disc. The observed tomogram of the flickering was compared with simulations, suggesting that the most intense flickering source in the H-alpha is not located in the accretion disc. It is proposed that the main line flickering source may be associated with the illuminated secondary star. Download/Website: http://arxiv.org/abs/astro-ph/0702308 Contact: [email protected] 2 ABSTRACTS OF REFEREED PAPERS 11

SWSextantis stars: the dominant population of CVs with orbital periods between 3–4 hours P. Rodr´ıguez-Gil1,2, B. T. Gansicke¨ 2, H.-J. Hagen3, S. Araujo-Betancor1, A. Aungwerojwit2,4, C. Allende Prieto5, D. Boyd6, J. Casares1, D. Engels3, O. Giannakis7, E. T. Harlaftis8, J. Kube9, H. Lehto10,11, I. G. Mart´ınez-Pais1,12 R. Schwarz13, W. Skidmore14, A. Staude13, M. A. P. Torres15 1 Instituto de Astrof´ısica de Canarias, V´ıa L´actea s/n, La Laguna, E-38205, Santa Cruz de Tenerife, Spain 2 Department of Physics, University of Warwick, Coventry CV4 7AL, UK 3 Hamburger Sternwarte, Universit¨at Hamburg, Gojenbergsweg 112, 21029 Hamburg, Germany 4 Department of Physics, Faculty of Science, Naresuan University, Phitsanulok, 65000, Thailand 5 McDonald Observatory and Department of Astronomy, University of Texas, Austin, TX 78712, USA 6 British Astronomical Association, Section, West Challow, OX12 9TX, England, UK 7 Institute of Astronomy and Astrophysics, National Observatory of Athens, P.O. Box 20048, Athens 11810, Greece 8 Institute of Space Applications and Remote Sensing, National Observatory of Athens, PO Box 20048, Athens 11810, Greece 9 Alfred-Wegener-Institut f¨ur Polar- und Meeresforschung, B¨urgermeister-Smidt-Straße 20, 27568 Bremerhaven, Germany 10 Tuorla Observatory, University of Turku, FIN-21500 Piikki¨o, Finland 11 Department of Physics, FIN-20014 University of Turku, Finland 12 Departamento de Astrof´ısica, Universidad de La Laguna, Tenerife, Spain 13 Astrophysikalisches Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany 14 California Institute of Technology, Mail Code 105-24, Pasadena, CA 91125-24, USA 15 Harvard-Smithsonian Center for Astrophysics, 60 Garden St, Cambridge, MA 02138, US Monthly Notices of the Royal Astronomical Society, in press (arxiv:0704.1129)

We present time-series optical photometry of five new CVs identified by the Hamburg Quasar Survey. The deep eclipses observed in HS 0129+2933 (= TT Tri), HS 0220+0603, and HS 0455+8315 provided very accurate orbital periods of 3.35129827(65), 3.58098501(34), and 3.56937674(26) h, respectively. HS 0805+3822 shows grazing eclipses and has a likely orbital period of 3.2169(2) h. Time-resolved optical spectroscopy of the new CVs (with the exception of HS 0805+3822) is also presented. Radial velocity studies of the Balmer emission lines provided an orbital period of 3.55 h for HS 1813+6122,which allowed us to identify the observed photometric signal at 3.39 h as a negative superhump wave. The spectroscopic behaviour exhibited by all the systems clearly identifies them as new SW Sextantis stars. HS 0220+0603 shows unusual N II and Si II emission lines suggesting that the donor star may have experienced nuclear evolution via the CNO cycle. These five new additions to the class increase the number of knownSW Sex stars to 35. Almost 40 per cent of the total SW Sex population do not show eclipses, invalidating the requirement of eclipses as a defining characteristic of the class and the models based on a high orbital inclination geometry alone. On the other hand, as more SW Sex stars are identified, the predominance of orbital periods in the narrow 3–4.5 h range is becoming more pronounced.In fact, almost half the CVs which populate the 3–4.5 h period interval are definite members of the class. The dominance of SW Sex stars is even stronger in the 2–3 h period gap, where they make up 55 per cent of all known gap CVs. These statistics are confirmed by our results from the Hamburg Quasar Survey CVs. Remarkably, 54 per cent of the Hamburg nova-like variables have been identified as SW Sex stars with orbital periods in the 3–4.5 h range. The observation of this pile-up of systems close to the upper boundary of the period gap is difficult to reconcile with the standard theory of CV evolution, as the SW Sex stars are believed to have the highest mass transfer rates among CVs. Finally, we review the full range of common properties that the SW Sex stars exhibit. Only a comprehensive study of this rich phenomenology will prompt to a full understandingof the phenomenonand its impact on the evolution of CVs and the accretion processes in compact binaries in general. Download/Website: http://uk.arxiv.org/abs/0704.1129 Contact: [email protected] 2 ABSTRACTS OF REFEREED PAPERS 12

XMM-Newton observations of EF Eridani: the textbook example of low-accretion rate polars A.D. Schwope1, A. Staude1, D. Koester2, J. Vogel1 1 Astrophysikalisches Institut Potsdam, An der Sternwarte 16, D-14482 Potsdam, Germany 2 Institut f¨ur Theoretische Physik und Astrophysik, Universit¨at Kiel, 24098 Kiel, Germany Astronomy & Astrophysics, in press (astro-ph/0703561)

Archival X-ray observations of EF Eridani obtained in a low state revealed distinct X-ray detections at a luminosity 29 −1 LX ∼ 2 × 10 erg s , three orders of magnitude below its high state value. The plasma temperature was found to be as low as kT ∼ 2keV, a factor 10 below the high state. The X-ray/UV/IR spectral energy distribution suggests faint residual accretion rather than coronal emission as being responsible for the low-state X-ray emission. EF Eri thus showed a clear transition from being shock-dominated in the high state to be cyclotron-dominated in the low state. From the optical/UV spectral energy distribution we re-determine the photospheric temperature of the white dwarf to ∼10000K. Contrary to earlier claims, WD model atmospheres produce sufficient UV flux to reproduce the published GALEX flux and orbital modulation. Contact: [email protected]

Equipotential Surfaces and Lagrangian Points in Non-synchronous, Eccentric Binary and Planetary Systems J.F. Sepinsky, B. Willems, V. Kalogera Department of Physics and Astronomy, Northwestern University, 2145 Sheridan Road, Evanston, IL 60208 The Astrophysical Journal, in press (astro-ph/0612508)

We investigate the existence and properties of equipotential surfaces and Lagrangian points in non-synchronous, eccentric and planetary systems under the assumption of quasi-static equilibrium. We adopt a binary potential that accounts for non-synchronous rotation and eccentric , and calculate the positions of the La- grangian points as functions of the mass ratio, the degree of asynchronism, the , and the position of the stars or planets in their relative orbit. We find that the geometry of the equipotential surfaces may facilitate non-conservative mass transfer in non-synchronous, eccentric binary star and planetary systems, especially if the componentstars or planets are rotating super-synchronously at the periastron of their relative orbit. We also calculate the volume-equivalent radius of the as a function of the four parameters mentioned above. Contrary to common practice, we find that replacing the radius of a circular orbit in the fitting formula of Eggleton (1983) with the instantaneous distance between the components of eccentric binary or planetary systems does not always lead to a good approximation to the volume-equivalentradius of the Roche-lobe. We therefore provide generalized analytic fitting formulae for the volume-equivalent Roche lobe radius appropriate for non-synchronous, eccentric binary star and planetary systems. These formulae are accurate to better than 1% throughout the relevant 2-dimensional parameter space that covers a dynamic range of 16 and 6 orders of magnitude in the two dimensions. Contact: [email protected] 2 ABSTRACTS OF REFEREED PAPERS 13

Spectroscopy of Nine Cataclysmic Variable Stars H. A. Sheets1, J. R. Thorstensen1, C. J. Peters1, A. B. Kapusta1, & C. J. Taylor2 1 Dept. Physics and Astronomy, 6127 Wilder Lab, Hanover, NH 03755, USA 2 The Lawrenceville School, P.O. Box 6008, Lawrenceville, NJ 08648, USA Publications of the Astronomical Society of the Pacific, in press

We present optical spectroscopy of nine cataclysmic binary stars, mostly dwarf novae, obtained primarily to deter- mine orbital periods Porb. The stars and their periods are LX And, 0.1509743(5) d; CZ Aql, 0.2005(6) d; LU Cam, 0.1499686(4) d; GZ Cnc, 0.0881(4) d; V632 Cyg, 0.06377(8) d; V1006 Cyg, 0.09903(9) d; BF Eri, 0.2708804(4) d; BI Ori, 0.1915(5) d; and FO Per, for which Porb is either 0.1467(4) or 0.1719(5) d. Several of the stars proved to be especially interesting. In BF Eri, we detect the absorption spectrum of a secondary star of spectral type K3 ±1 subclass, which leads to a distance estimate of ∼ 1 kpc. However, BF Eri has a large (∼ 100 mas yr−1), and we have a preliminary measurement that confirms the large proper motion and yields only an upper limit for the parallax. BF Eri’s space velocity is evidently large, and it appears to belong to the halo population. In CZ Aql, the emission lines have strong wings that move with large velocity amplitude, suggesting a magnetically-channeled accretion flow. The orbital period of V1006 Cyg places it squarely within the 2- to 3- ‘gap’ in the distribution of cataclysmic binary orbital periods. Download/Website: http://xxx.lanl.gov/abs/0704.0948 Contact: [email protected]

On the effect of emission lines on the UBVR photometry A. Skopal Astronomical Institute, Slovak Academy of Sciences, 059 60 Tatransk´aLomnica, Slovakia New Astronomy, in press

We investigate the effect on the U, B, V, RC and RJ magnitudes of the removal of emission lines from a spectrum. We determined ∆m corrections from the ratio of fluxes with and without emission lines, transmitted from the object through the photometric filter. An exact and a simplified approach for operative use were applied. The effect was demonstrated for classical symbiotic stars, symbiotic novae and the classical nova V1974Cyg. It was found that about 20-30%, 30-40%, 10% and 26/20% of the observed flux in the U, B, V and RC/RJ filter, respectively, is radiated in the emission lines of the investigated classical symbiotic stars. The largest effect was found for symbiotic novae (RRTel and V1016Cyg) and the classical nova V1974Cyg at 210 days (in average of 74%, 79%, 56% and 66/60%), because of their very strong emission line spectrum. In all cases the line corrected flux-points fit well the theoretical continuum. The difference between ∆m corrections obtained by the accurate calculation and that given by our approximate formula is less than 10%. Deviations up to 30% can be only in the U passband. Examples for practical application are suggested. Download/Website: http://www.astro.sk/ astrskop/ubvr.corr/ Contact: [email protected] 2 ABSTRACTS OF REFEREED PAPERS 14

Comprehensive simulations of superhumps Amanda J. Smith1, Carole A. Haswell1, James R. Murray2, Michael R. Truss3, Stephen B. Foulkes1 1 Department of Physics and Astronomy, The Open University, Walton Hall, Milton Keynes, MK7 6AA, UK 2 Department of Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, VIC 3122, Australia 3 Department of Physics, Durham University, South Road, Durham, DH1 3LE, UK 11, Monthly Notices of the Royal Astronomical Society, in press (astro-ph/0704.1519)

We use 3D SPH calculations with higher resolution, as well as with more realistic viscosity and sound-speed pre- scriptions than previous work to examine the eccentric instability which underlies the superhump phenomenon in semi-detached binaries. We illustrate the importance of the two-armed spiral mode in the generation of superhumps. Differential motions in the fluid disc cause converging flows which lead to strong spiral shocks once each super- hump cycle. The dissipation associated with these shocks powers the superhump. We compare 2D and 3D results, and conclude that 3D simulations are necessary to faithfully simulate the disc dynamics. We ran our simulations for unprecedented durations, so that an eccentric equilibrium is established except at high mass ratios where the growth rate of the instability is very low. We collate the observed data on superhumps. Our improved simulations give a closer match to the observed rela- tionship between superhump period excess and binary mass ratio than previous numerical work. The observed black hole X-ray transient superhumpers appear to have systematically lower disc precession rates than the cataclysmic variables. This could be due to higher disc temperatures and thicknesses. No high-resolution 3D disc with mass ratio q > 0.24 developed superhumps, in agreement with analytical expectations. The modulation in total viscous dissipation on the superhump period is overwhelmingly from the region of the disc within the 3 : 1 resonance radius. The precession rates of our high resolution 3D discs match the single particle dynamical precession rate at 0.87R3:1. As the eccentric instability develops, the viscous torques are enhanced, and the disc consequently adjusts to a new equilibrium state, as suggested in the thermal-tidal instability model. We quantify this enhancement in the viscosity, which is ∼ 10 per cent for q = 0.08. The disc motions can be described as superpositions of the S(k,l) modes, and the disc executes complex standing wave dynamics which repeat in the inertial frame on the disc precession period. We characterise the eccentricity distributions in our accretion discs, and show that the entire body of the disc partakes in the eccentricity. Download/Website: http://arxiv.org/abs/0704.1519 Contact: [email protected]

SDSS J233325.92+152222.1 and the evolution of intermediate polars John Southworth1,B.T.Gansicke¨ 1, T. R. Marsh1, D. de Martino2,A. Aungwerojwit1,3 1 University of Warwick, Coventry, CV4 7AL, UK 2 INAF – Osservatorio di Capodimonte, Via Moiariello 16, 80131 Napoli, Italy 3 Department of Physics, Faculty of Science, Naresuan University, Phitsanulok, 60500, Thailand Monthly Notices of the Royal Astronomical Society, in press (arXiv:0704.1570)

Intermediate polars (IPs) are cataclysmic variables which contain magnetic white dwarfs with a rotational period shorter than the binary orbital period. Evolutionary theory predicts that IPs with long orbital periods evolve through the 2–3hr period gap, but it is very uncertain what the properties of the resulting objects are. Whilst a relatively large number of long-period IPs are known, very few of these have short orbital periods. We present phase-resolved spectroscopy and photometry of SDSSJ233325.92+152222.1 and classify it as the IP with the shortest known orbital period (83.12±0.09min), which contains a white dwarf with a relatively long spin period (41.66±0.13min). 33 3 We estimate the white dwarf’s magnetic moment to be µWD ≈ 2 × 10 Gcm , which is not only similar to three of the other four confirmed short-period IPs but also to those of many of the long-period IPs. We suggest that long- period IPs conserve their magnetic moment as they evolve towards shorter orbital periods. Therefore the dominant 2 ABSTRACTS OF REFEREED PAPERS 15 population of long-period IPs, which have white dwarf spin periods roughly ten times shorter than their orbital periods, will likely end up as short-period IPs like SDSS J2333, with spin periods a large fraction of their orbital periods. Download/Website: http://arxiv.org/abs/0704.0513 Contact: [email protected]

Cataclysmic Variables from SDSS VI. The Sixth Year (2005) P. Szkody1, A. Henden2, L. Mannikko1, A. Mukadam1, G. D. Schmidt3, J. J. Bochanski1, M. Agueros¨ 1, S. F. Anderson1, N. M. Silvestri1, W. E. Dahab4, M. Oguri4,5, D. P.Schneider6, M.-S. Shin4, M. A. Strauss4, G. R.Knapp4, A. A. West1 1 Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195, USA 2 US Naval Observatory, Flagstaff Station, P. O. Box 1149, Flagstaff, AZ 86002-1149 and AAVSO, 49 Bay State Rd, Cambridge, MA 02138, USA 3 The University of Arizona, Steward Observatory, Tucson, AZ 85721, USA 4 Princeton University Observatory, Peyton Hall, Princeton, NJ 08544, USA 5 Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, 2575 Sand Hill Road, Menlo Park, CA 94025, USA 6 Department of Astronomy and Astrophysics, 525 Davey Laboratory, Pennsylvania State University, University Park, PA 16802, USA The Astronomical Journal, in press

The 28 cataclysmic variables found in 2005 in the Sloan Digital Sky Survey are presented with their coordinates, magnitudes and spectra. Five of these systems are previously known CVs (HH Cnc, SX LMi, QZ Ser, AP CrB and HS1016+3412) and the rest are new discoveries. Additional spectroscopic, photometric and/or polarimetric observations of 10 systems were carried out, resulting in estimates of the orbital periods for seven of the new binaries. The 23 new CVs include one eclipsing system, one new Polar and five systems whose spectra clearly reveal atmospheric absorption lines from the underlying white dwarf. Download/Website: http://www.astro.washington.edu/szkody/papers/sloan6.ps Contact: [email protected]

On the orbital period of the magnetic Cataclysmic Variable HS 0922+1333 G. H. Tovmassian, S.V. Zharikov Observatorio Astr´onomico Nacional SPM, Instituto de Astronom´ıa, Universidad Nacional Aut´onoma de M´exico, Ensenada, BC, M´exico Astronomy & Astrophysics, in press (arXiv:0704.0961v1)

The object HS0922+1333was visited briefly in 2002 in a mini survey of low accretion rate polars (LARPs) in order to test if they undergo high luminosity states similar to ordinary polars. On the basis of that short observation the suspicion arose that the object might be an asynchronous polar (Tovmassian et al 2004). The disparity between the presumed orbital and spin period appeared to be quite unusual. We performedfollow-up observationsof the object to resolve the problem. New simultaneous spectroscopic and photometric observations spanning several years allowed measurements of radial velocities of emission and absorption lines from the secondary star and brightness variations due to synchrotron emission from the primary. New observations show that the object is actually synchronous and its orbital and spin period are equal to 4.04 hours. We identify the source of confusion of previous observations to be a high velocity component of emission line arousing from the stream of matter leaving L1 point. Contact: [email protected]/[email protected] 3 ABSTRACTS OF THESES 16

3 Abstracts of theses Mass Transfer and Evolution of Compact Binary Stars Vayujeet Gokhale Department of Physics & Astronomy, Louisiana State University, Baton Rouge, LA 70803-4001 Thesis Abstract, published (2007PhDT...... 1G)

We present a study of the key aspects of the evolution of binary stars with emphasis on binaries consisting of two white dwarf stars. The evolution of such systems is driven by the loss of angular momentum by gravitational wave radiation. Effects like mass transfer and other modes of angular momentum loss and redistribution influence the evolutionary fate of the binary, and can lead to a merger, the tidal disruption of one of the components or its survival as a long-lived AM Canum Venaticorum (AM CVn) type system. Our study takes into account some of these effects; like mass loss, tides, accretion disk formation and direct impact accretion. We find that under some circumstances, the tidal coupling between the spin of the components and the orbit of the binary leads to oscillations in the orbital separation and the mass transfer rate. We also find that as compared to previous studies, a larger fraction of the systems should survive to form AM CVn type systems. We also consider systems in which the mass transfer rate exceeds the critical Eddington rate, leading to mass loss from the system. It is possible that some of the lost mass settles into a disk around the binary to form a circumbinary disk. In the second part of the thesis, we present a toy model for disks in general, and find that the coupling such a circumbinary disk to the binary has a destabilizing effect on the binary. Download/Website: http://gawaine.phys.lsu.edu/gokhale Contact: [email protected]

4 As seen on astro-ph

As in the past, we compile here literature “as seen on astro-ph” on / relevant to binary star research, grouped into a number of topics. Due to a disastrous error that occurred to one of the editors [BG], we published in the last issue not the astro-ph summary of the preceeding months, but a copy of the list from IBNews #25. Taking the risk that some of the material below is somewhat out of date, we decided nevertheless to include in this issue the list that was scheduled for #27 as well as the list for #28 i.e. from December 2006 to April 2007. Please note that the astro-ph identifier changed as of 1 April 2007.

4.1 Cataclysmic Variables and related systems astro-ph/0611026: Spitzer IRS Spectroscopy of Intermediate Polars: Constraints on Mid-Infrared Cyclotron Emission by Thomas E. Harrison et al. astro-ph/0611117: ULTRACAM Photometry of the ultracompact binaries V407 Vul and HM Cnc by S.C.C. Barros et al. astro-ph/0611154: A Thousand and One Nova Outbursts by N. Epelstain et al. astro-ph/0611200: Magnetically moderated outbursts of WZ Sagittae by O.M. Matthews et al. astro-ph/0611267: Determination of the basic parameters of the dwarf nova EY Cygni by J. Echevarria et al. astro-ph/0611268: Proof of polar ejection fom the close-binary core of the planetary Abell 63 by Deb- orah L. Mitchell et al. astro-ph/0611461: Understanding white dwarf binary evolution with white dwarf/main sequence binaries: first results from SEGUE by M.R. Schreiber, A. Nebot Gomez-Moran, A.D. Schwope 4 AS SEENON ASTRO-PH 17 astro-ph/0611475: Evidence for bipolar jets from the optical spectra of the prototypical symbiotic star Z An- dromedae by Mari Burmeister, Laurits Leedjarv astro-ph/0611758: An in-depth study of the pre-polar candidate WX LMi by J. Vogel, A.D. Schwope, B.T. Gaensicke astro-ph/0611825: Discovery of thirteen novae candidates in M87 by Juan P. Madrid et al. astro-ph/0611829: Spectroscopic search for new SW Sextantis stars in the 3-4 hour orbital period range – I by P. Rodriguez-Gil, L. Schmidtobreick, B. T. Gaensicke astro-ph/0611933: The Incidence of Dwarf Novae in Large Area Transient Searches by A. Rau et al. astro-ph/0612099: Interferometric Observations of RS Ophiuchi and the Origin of the Near-IR Emission by B. F. Lane et al. astro-ph/0612220: A brown dwarf mass donor in an accreting binary by S.P. Littlefair et al. astro-ph/astro-ph/0612251: An alternative to common envelope evolution by Martin E. Beer et al. astro-ph/0612298: A Photometric and Spectroscopic Study of the Cataclysmic Variable ST LMi during 2005- 2006 by S. Kafka et al. astro-ph/0612502: Bipolar ejection by the system Z And during its 2006 outburst by N. A. Tomov et al. astro-ph/0612529: HST and Optical Observations of Three Pulsating Accreting White Dwarfs in Cataclysmic Variables by Paula Szkody et al. astro-ph/0612532: The B + white dwarf binary KPD 1930+2752 - a Supernova Type Ia progenitor candidate by S. Geier et al. astro-ph/0612596: X-ray monitoring of optical novae in M31 from July 2004 to February 2005 by W. Pietsch et al. astro-ph/0612657: A Synthetic Spectrum and Light Curve Analysis of the Cataclysmic Variable IX Velo- rum by Albert P. Linnell et al. astro-ph/0612692: An Illustration of Modeling Cataclysmic Variables: HST, FUSE, SDSS Spectra of SDSSJ080908.39+381406.2 by Albert P. Linnell et al. astro-ph/0612696: MV Lyrae in Low, Intermediate, and High States by Albert P. Linnell et al. astro-ph/0701025: Hard X-ray and Infrared Emission from Apparently Single White Dwarfs by Y.-H. Chu et al. astro-ph/0701307: Spitzer Space Telescope observations of magnetic cataclysmic variables: possibilities for the presence of dust in polars by C. S. Brinkworth et al. astro-ph/0701336: Discovery of Rapid Hard X-ray Variability and New Jet Activity in the Symbiotic Binary R Aqr by J. S. Nichols et al. astro-ph/0701404: HST and VLT observations of the Symbiotic Star Hen 2-147 by M. Santander-Garcia et al. astro-ph/0701560: DE CVn: A bright, eclipsing - white dwarf binary by E.J.M. van den Besselaar et al. astro-ph/0701572: The statistical significance of the superhump signal in U Gem by Matthias R. Schreiber astro-ph/0701654: Cataclysmic Variables by Robert Connon Smith astro-ph/0702754: Cool Companions to White Dwarf Stars from the Two Micron All Sky Survey All Sky Data Release by D. W. Hoard et al. astro-ph/0702005: The mass and radius of the M-dwarf in the short period eclipsing binary RR Caeli by P.F.L. Maxted et al. astro-ph/0702049: Thermally Stable Nuclear Burning on Accreting White Dwarfs by Ken J. Shen & Lars Bildsten astro-ph/0702129: Photometry of VS0329+1250: A New, Short-Period SU Ursae Majoris Star by A. W. Shafter et al. astro-ph/0702308: Emission Line Flickering from the Secondary Star in Cataclysmic Variables? A study of V3885 Sagitarii by Fabiola M. A. Ribeiro & Marcos P. Diaz 4 AS SEENON ASTRO-PH 18 astro-ph/0702367: Chandra High Resolution X-ray Spectroscopy of AM Her by V. Girish et al. astro-ph/0702374: A compact dust shell in the symbiotic system HM Sge by Stephane Sacuto et al. astro-ph/0702388: The Stability of Double White Dwarf Binaries Undergoing Direct Impact Accretion by Patrick M. Motl et al. astro-ph/0702419: Two SMC Symbiotic stars undergoing steady hydrogen burning by M. Orio et al. astro-ph/0702563: A Universal Decline Law of Classical Novae. II. GK Persei 1901 and Novae in 2005 by Izumi Hachisu & Mariko Kato astro-ph/0702607: Analysis of the first confirmed superoutburst of V337 Cygni in 2006 May by David Boyd et al. astro-ph/0702640: On the contribution of point sources to the Galactic ridge X-ray emission by M.Revnivtsev et al. astro-ph/0702662: Population Synthesis Studies of Close Binary Systems Using a Variable Common Envelope Efficiency Parameter: I. Dependence upon Secondary Mass by Michael Politano & Kevin P. Weiler astro-ph/0702752: Long-term monitoring of the short period SU UMa-type dwarf nova, V844 Herculis by Shota Oizumi et al. astro-ph/0703041: Hubble Space Telescope Far Ultraviolet Spectroscopy of the Dwarf Nova VW Hyi in Super- outburst by Jason Merritt et al. astro-ph/0703083: A Far Ultraviolet Study of the Nova-like V794 Aquilae by P. Godon et al. astro-ph/0703087: The Masses and Evolutionary State of the Stars in the Dwarf Nova SS Cygni by Martin A. Bitner et al. astro-ph/0703185: Supersoft X-ray Light Curve of RS Ophiuchi (2006) by Izumi Hachisu et al. astro-ph/0703278: CH Cyg X-ray Jet Activity and Multi-component Structures by M. Karovska et al. astro-ph/0703286: Swift X-ray Observations of Classical Novae by J.-U. Ness et al. astro-ph/0703464: Spitzer Space Telescope Observations of the Magnetic Cataclysmic Variable AE Aqr by G. Dubus et al. astro-ph/0703561: XMM-Newton observations of EF Eridani: the textbook example of low-accretion rate po- lars by A.D. Schwope et al. astro-ph/0703578: Faint Thermonuclear Supernovae from AM Canum Venaticorum Binaries by Lars Bildsten et al. astro-ph/0703763: First detection of Zeeman absorption lines in the polar VV Pup by E. Mason et al. astro-ph/0704.0017: Spectroscopic Observations of the EX Hydrae in Quiescence by Nceba Mhlahlo et al. astro-ph/0704.0280: Common Envelope Evolution Redux by Ronald F. Webbink astro-ph/0704.0513: SDSS J233325.92+152222.1 and the evolution of intermediate polars by John Southworth et al. astro-ph/0704.0789: New Close Binary Systems from the SDSS-I (Data Release Five) and the Search for Mag- netic White Dwarfs in Cataclysmic Variable Progenitor Systems by Nicole M. Silvestri et al. astro-ph/0704.0948: Spectroscopy of Nine Cataclysmic Variable Stars by H. A. Sheets et al. astro-ph/0704.0961: On the orbital period of the magnetic Cataclysmic Variable HS 0922+1333 by G. H. Tovmassian et al. astro-ph/0704.1129: SW Sextantis stars: the dominant population of CVs with orbital periods between 3-4 hours by P. Rodriguez-Gil et al. astro-ph/0704.1133: FUSE Observations of the Dwarf Novae UU Aql, BV Cen, and CH UMa in Quiescence by Edward M. Sion et al. astro-ph/0704.1276: SDSS J102146.44+234926.3: New WZ Sge-type dwarf nova by Alex Golovin et al. astro-ph/0704.1302: Photometry of the SW Sex-type nova-like BH Lyncis in high state by V. Stanishev et al. astro-ph/0704.1388: Why do some intermediate polars show soft X-ray emission? A survey of XMM-Newton spectra by P. A. Evans & Coel Hellier 4 AS SEENON ASTRO-PH 19 astro-ph/0704.1641: U Geminorum: a test case for orbital parameters determination by J. Echevarria et al. astro-ph/0704.2240: Hydrodynamical simulations of the jet in the symbiotic star MWC 560 III. Application to X-ray jets in symbiotic stars by Matthias Stute & Raghvendra Sahai astro-ph/0704.2549: Swift observations of the 2006 outburst of the recurrent nova RS Ophiuchi: II. 1D hydro- dynamical models of wind driven shocks by N. M. H. Vaytet et al. astro-ph/0704.2836: An International Ultraviolet Explorer Archival Study of Dwarf Novae in Outburst by Ryan T.Hamilton et al. astro-ph/0704.3166: XMM-Newton observations of Nova Sgr 1998 by M. Hernanz & G. Sala astro-ph/0704.3168: Detection of superhumps in the VY Scl-type nova-like variable KR Aur by V. P. Kozhevnikov astro-ph/0704.3507: The Clusters AgeS Experiment (CASE). I. V209 omega Cen - An Eclipsing Post-Common Envelope Binary in the omega Cen by J. Kaluzny et al.

4.2 LMXBs and related systems astro-ph/0611049: First e-VLBI observations of GRS 1915+105 by A. Rushton et al. astro-ph/0611050: The first detection of Compton Reflection in the Low-Mass X-ray Binary 4U1705-44 with INTEGRAL and BeppoSAX by Mariateresa Fiocchi et al. astro-ph/0611054: First e-VLBI observations of Cygnus X-3 by V. Tudose et al. astro-ph/0611057: Jet-powered optical nebulae from X-ray binaries by David M. Russell et al. astro-ph/0611064: Hard X-ray emission of the microquasar GX 339-4 in the low/hard state by A. Joinet et al. astro-ph/0611076: Type I X-ray Bursts at Low Accretion Rates by Fang Peng, Edward F. Brown, James W. Truran astro-ph/0611107: Spectral variability modes of GX 339-4 in a hard-to-soft state transition by M. Del Santo et al. astro-ph/0611111: Monitoring LMXBs with the Faulkes Telescope by Fraser Lewis et al. astro-ph/0611177: Galactic centre X-ray sources by Andrew J. Gosling, Reba M. Bandyopadhyay, Katherine M. Blundell astro-ph/0611179: Energy spectra of X-ray quasi-periodic oscillations in accreting black hole binaries by P.T. Zycki, M.A. Sobolewska, A. Niedzwiecki astro-ph/0611218: An integral monitoring of GRS1915+105: simultaneous observations with INTEGRAL, RXTE, the Ryle and Nancay radio telescopes by J. Rodriguez et al. astro-ph/0611219: An INTEGRAL monitoring of GRS 1915+105 using simultaneous space and ground based instruments by Jerome Rodriguez et al. astro-ph/0611235: Low mass X-ray binaries with pre-main sequence companions by Natalia Ivanova astro-ph/0611237: The Low-Mass X-ray Binary and Globular Cluster Connection in Virgo Cluster Early-type : Optical Properties by Gregory R. Sivakoff et al. astro-ph/0611256: Fast aperiodic variability in the black hole binary GRS 1915+105: the timing signature of relativistic ejection events by P. Soleri, T. Belloni, P. Casella astro-ph/0611341: The discovery outburst of the X-ray transient IGR J17497-2821 observed with RXTE and ATCA by Jerome Rodriguez et al. astro-ph/0611344: Hunting the nature of IGR J17497-2821 with X-ray and NIR observations by A. Paizis et al. astro-ph/0611375: RXTE observations of the Low/Hard State X-ray Outburst of the new x-ray transient SWIFT J1753.5-0127 by M.C. Ramadevi, S. Seetha astro-ph/0611380: New outbursts of the black hole candidate H1743-322/IGR J17464-3213 observed by IN- TEGRAL by F. Capitanio et al. astro-ph/0611399: INTEGRAL and RXTE observations of the fast X-ray transient XTEJ1901+014 by D. I. 4 AS SEENON ASTRO-PH 20

Karasev, A. A. Lutovinov, S. A. Grebenev astro-ph/0611628:A unified paradigm for the spectral and temporal evolution of Black Hole X-ray Binaries by P. O. Petrucci et al. astro-ph/0611713: Simultaneous radio/X-ray observations of Cir X-1 by V. Tudose et al. astro-ph/0611716: Evidence for 1122 Hz X-Ray Burst Oscillations from the Neutron-Star X-Ray Transient XTE J1739-285 by P. Kaaret et al. astro-ph/0611823: High-resolution X-ray spectroscopy of the ultracompact LMXB 4U 1626-67 by Miriam I. Krauss et al. astro-ph/0611889: Origin of Superluminal radio jets in GRS 1915+105 and the role of the Plateau state by JS Yadav astro-ph/0611909: The Galactic Black Holes Cyg X-1, GX 339-4, and 4U 1957+11: In Transition and at High Resolution by Michael A. Nowak astro-ph/0612007: Determining the nature of the faint X-ray source population near the Galactic Centre by Reba M. Bandyopadhyay et al. astro-ph/0612050: Black Hole Formation in X-Ray Binaries: The Case of XTE J1118+480 by T. Fragos et al. astro-ph/0612058: Low-Mass X-ray Binaries and Globular Clusters in Early-Type Galaxies. I. Chandra Ob- servations by Philip J. Humphrey & David A. Buote astro-ph/0612093: Order in the Chaos: Spin-up and Spin-down during the 2002 Outburst of SAX J1808.4- 3658 by L. Burderi et al. astro-ph/0612129: Millisecond Dips in Sco X-1 are Likely the Result of High-Energy Particle Events by T. A. Jones et al. astro-ph/0612178: On the nature of X-Ray Flashes in the SWIFT era by B. Gendre et al. astro-ph/0612211: Evidence for deceleration in the radio jets of GRS1915+105? by J.C.A. Miller-Jones et al. astro-ph/0612232: Constraints on Thermal X-ray Radiation from SAX J1808.4-3658 and Implications for Neutron Star Neutrino Emission by C. O. Heinke et al. astro-ph/0612236: Simulations of the Disk-Jet Interaction in GRS 1915+105 and Other Systems by David M. Rothstein astro-ph/0612269: Chandra Observation of the Big Dipper X 1624-490 by R. Iaria et al. astro-ph/0612302: Discovery of a New X-Ray Burst/Millisecond Accreting Pulsar HETE J1900.1-2455 by M. Suzuki et al. astro-ph/0612312: Observational evidence for stellar-mass black holes by Jorge Casares astro-ph/0612431: A detection of the donor star of Aquila X-1 during its 2004 outburst? by R. Cornelisse et al. astro-ph/0612461: Kerr Parameters a* for GRO J1655-40and 4U 1543-47,and their Consequences; Modelling GRS 1915+105 by G.E. Brown et al. astro-ph/0612575: Simultaneous multiwavelength observations of the Low/Hard State of the X-ray transient source SWIFT J1753.5-0127 by M. Cadolle Bel et al. astro-ph/0612592: Chandra Observation of the Dipping Source XB 1254-690 by R. Iaria et al. astro-ph/0612611: Constraints on Braneworld Models from a Kinematic Limit on the Age of the Black Hole XTE J1118+480 by Dimitrios Psaltis astro-ph/0612675: Power spectra of black holes and neutron stars as a probe of hydrodynamical structure of the source. Diffusion theory and its application to Cyg X-1 and Cyg X-2 X-ray observations by Lev Titarchuk et al. astro-ph/0612680: Is the Lack of Pulsations in Low Mass X-Ray Binaries due to Comptonizing Coronae? by Ersin Gogus et al. astro-ph/0612789: Testing consistency of deconfinement heating of strange stars in superbursters and soft X-ray transients by M. Stejner astro-ph/0612790: A precessing warped accretion disk around the X-ray pulsar Her X-1 by D. Klochkov et al. astro-ph/0612791: Constraints on Neutron Star Properties from X-ray Observations of Millisecond Pulsars by 4 AS SEENON ASTRO-PH 21

Slavko Bogdanov et al. astro-ph/0701077: Variability of Nineteen Millisecond Pulsars in 47 Tucanae with CHANDRA/HRC-S by P. B. Cameron et al. astro-ph/0701244: The INTEGRAL Galactic bulge monitoring program: the first 1.5 years by E. Kuulkers et al. astro-ph/0701312: Supporting evidence for the signature of the innermost stable circular orbit in Rossi X-ray data from 4U1636-536 by Didier Barret et al. astro-ph/0701470: The superorbital variability and triple nature of the X-ray source 4U 1820-303 by A. A. Zdziarski et al. astro-ph/0701472: Dependence of the orbital modulation of X-rays from 4U 1820-303 on the accretion rate by A. A. Zdziarski et al. astro-ph/0701575: Discovery of X-ray burst triplets in EXO 0748-676 by L. Boirin et al. astro-ph/0701708: The Latitude of Type I X-Ray Burst Ignition on Rapidly Rotating Neutron Stars by Randall L. Cooper & Ramesh Narayan astro-ph/0701810: Six new candidate ultracompact X-ray binaries by J.J.M. in ’t Zand et al. astro-ph/0701850: Millisecond dips in the RXTE/PCA light curve of Sco X-1 and TNO occultation by Hsiang- Kuang Chang et al. astro-ph/0701865: Using the X-ray Dust Scattering Halo of 4U 1624-490 to determine distance and dust dis- tributions by Jingen Xiang et al. astro-ph/0701915: On the ultra-compact nature of 4U1822-000 by T. Shahbaz et al. astro-ph/0702042: Hydrogen-Triggered Type I X-ray Bursts in a Two-Zone Model by Randall L. Cooper & Ramesh Narayan astro-ph/0702087: Clear anti-correlation between luminosity and high energy cutoff in the low/hard state of the black hole candidate GX339-4 by Takehiro G. Miyakawa et al. astro-ph/0702089: Evaluating Spectral Models and the X-ray States of Neutron-Star X-ray Transients by Dacheng Lin et al. astro-ph/0702157: On the kHz QPO frequency correlations in bright neutron star X-ray binaries by T. Belloni et al. astro-ph/0702200: X-Ray Spectral Variability in Initial Rise of XTE J1550-564 by Y. X. Wu et al. astro-ph/0702263: Study of the Fast X-Ray Transient XTE J1901+014 Based on INTEGRAL, RXTE and ROSAT Data by D.I.Karasev, A.A.Lutovinov, S.A.Grebenev (Space Research Institute, Moscow, Russia) astro-ph/0702454: Accreting X-ray millisecond pulsars observed with INTEGRAL by Maurizio Falanga astro-ph/0702490: Discovery of a flux-related change of the cyclotron line energy in Her X-1 by R.Staubert et al. astro-ph/0702528: Long-term developments in Her X-1: Correlation between the histories of the 35 turn- on cycle and the 1.24 sec pulse period by R. Staubert et al. astro-ph/0702536: A 0535+26 in the August/September 2005 outburst observed by RXTE and INTEGRAL by I. Caballero et al. astro-ph/0702624: The hard X-ray tails in neutron star low mass X-ray binaries: BeppoSAX observations and possible theoretical explanation of the GX 17+2 case by R. Farinelli et al. astro-ph/0702690: Generation of Type I X-ray Burst Oscillations by Unstable Surface Modes by Ramesh Narayan & Randall L. Cooper astro-ph/0703020: The quasi-persistent neutron star soft X-ray transient 1M 1716-315 in quiescence by P.G. Jonker et al. astro-ph/0703074: Anti-correlated hard X-ray time lags in Galactic black hole sources by K. Sriram et al. astro-ph/0703092: Probing the Formation of Low Mass X-ray Binaries in Globular Clusters and the Field by Arunav Kundu et al. astro-ph/0703170: Coupling between the 45 Hz Horizontal-Branch Oscillation and the Normal Branch Oscil- 4 AS SEENON ASTRO-PH 22

lation in Scorpius X-1 by Wenfei Yu astro-ph/0703203: Burial of the polar magnetic field of an accreting neutron star. II. Hydromagnetic stability of axisymmetric equilibria by D. J. B. Payne & A. Melatos astro-ph/0703274: Periodicities in X-ray Binaries from Swift/BAT Observations by R. Corbet et al. astro-ph/0703287: Limits on Mass and Radius for the ms-Period X-ray Pulsar SAX J1808.4-3658 by Denis A. Leahy et al. astro-ph/0703311: Explosive hydrogen burning during type I X-ray bursts by Jacob Lund Fisker et al. astro-ph/0703384: Peak of the Hard States of GX 339-4: Implications for the Accretion Geome- try, Disk Mass, and Black Hole Mass by Wenfei Yu et al. astro-ph/0703431: Correlations between X-ray Spectral Characteristics and Quasi-Periodic Oscillations in Sco X-1 by Charles F. Bradshaw et al. astro-ph/0703497: Swift Observations of the Cooling Accretion Disk of XTE J1817-330 by E. S. Rykoff et al. astro-ph/0703501: Uncovering the Nature of the X-ray Transient 4U 1730-22: Discovery of X-ray Emission from a Neutron Star in Quiescence with Chandra by John A. Tomsick et al. astro-ph/0703692: GRO J1744-28, search for the counterpart: infrared photometry and spectroscopy by An- drew J. Gosling et al. astro-ph/0704.0267: Near-Infrared Spectra of the Black Hole X-Ray Binary, A0620-00 by C.S. Froning et al. astro-ph/0704.0689: Study on Correlations between the Twin Kilohertz Quasi-periodic Oscillations in Low- mass X-ray Binaries by H. X. Yin & Y. H. Zhao astro-ph/0704.0734: GRO J1655-40: from ASCA and XMM-Newton Observations by Xiao-Ling Zhang et al. astro-ph/0704.1741: Detection of a 1258 Hz high-amplitude kilohertz quasi-periodic oscillation in the ultra- compact X-ray binary 1A 1246-588 by P.G. Jonker et al. astro-ph/0704.2134: XMMU J174716.1-281048: a ”quasi-persistent” very faint X-ray transient? by M. Del Santo et al. astro-ph/0704.2318: On a multi-resonant origin of high frequency quasiperiodic oscillations in the neutron- star X-ray binary 4U 1636-53 by Zdenek Stuchlik et al. astro-ph/0704.3062: INTEGRAL observations of HER X-1 by D. Klochkov et al.

4.3 HMXBs and related systems astro-ph/0611025: Are the distances of galactic microquasars reliable? by C. Foellmi astro-ph/0611145: Modelling mid-Z element atmospheres for strongly-magnetized neutron stars by Kaya Mori, Wynn C.G. Ho astro-ph/0611166: Clues from microquasars to the origin of radio-loudness of quasars by Carlo Nipoti, Kather- ine M. Blundell, James Binney astro-ph/0611217: Broad-band spectral changes of the microquasars Cygnus X-1 and SWIFT J1753.5-0127 by Marion Cadolle Bel et al. astro-ph/0611343: The XMM-Newton/INTEGRAL monitoring campaign of IGR J16318-4848 by A.Ibarra et al. astro-ph/0611424: A Wolf-Rayet/black-hole X-ray binary candidate in NGC 300 by S. Carpano et al. astro-ph/0611477: X-ray broad-band study of the symbiotic X-ray binary 4U 1954+31 by N. Masetti et al. astro-ph/0611516: The Be/X-ray transient 4U 0115+63/V635 Cassiopeiae. III. Quasi-cyclic variability by P. Reig et al. astro-ph/0611558: Multi-wavelength observations of the microquasar XTE J1720-318: a transition from high- soft to low-hard state by Sylvain Chaty astro-ph/0611937: Observation Campaign of SS 433 in April 2006 by T. Kotani et al. astro-ph/0612318: Theoretical overview on high-energy emission in microquasars by V. Bosch-Ramon astro-ph/0701070: Chandra and XMM-Newton discovery of the transient X-ray pulsar in the nearby spiral 4 AS SEENON ASTRO-PH 23

NGC2403 by Sergey Trudolyubov et al. astro-ph/0701092: Lost and Found: A New Position and Infrared Counterpart for the X-ray Binary Scutum X-1 by D. L. Kaplan et al. astro-ph/0701095: Observations of the 599 Hz Accreting X-ray Pulsar IGR J00291+5934 during the 2004 Outburst and in Quiescence by M. A. P. Torres et al. astro-ph/0701144: Compactified pulsar wind nebula model of gamma-ray loud binary LSI +61 303 by A.Neronov & M.Chernyakova astro-ph/0701184: X-ray bright sources in the Chandra Small Magellanic Cloud Wing Survey - detection of two new pulsars by K. E. McGowan et al. astro-ph/0701645: The jet-powered optical nebula of Cygnus X-1 by D. M. Russell et al. astro-ph/0701743: Microquasars: disk-jet coupling in stellar-mass black holes by I.F. Mirabel astro-ph/0701791: INTEGRAL and Swift observations of EXO 2030+375 during a giant outburst by D. Klochkov et al. astro-ph/0701837: Microquasars: Progress made and open questions by I.F. Mirabel astro-ph/0702022: RXTE spectra of the Galactic microquasar GRO J1655-40 during the 2005 outburst by Koji Saito et al. astro-ph/0702059: On the abundances of GRO J1655-40 by C. Foellmi et al. astro-ph/0702142: Orbital Evolution and orbital phase resolved spectroscopy of the HMXB pulsar 4U 1538-52 with RXTE-PCA and BeppoSAX by U. Mukherjee et al. astro-ph/0702248: Finding Periods in High Mass X-Ray Binaries by Gordon E. Sarty et al. astro-ph/0702283: Joint H-alpha and X-Ray Observations of Massive X-Ray Binaries. III. The Be X-ray Bi- naries HDE 245770 = A 0535+26 and X Persei by E. D. Grundstrom et al. astro-ph/0702393: Recent Radio Monitoring of Microquasars with RATAN-600 Radio Telescope by S.A. Trushkin et al. astro-ph/0702477: IGR J18483-0311: an accreting X-ray pulsar observed by INTEGRAL by V. Sguera et al. astro-ph/0702688: Accreting corona model of the X-ray variability in soft state X-ray binaries and active galactic nuclei by A. Janiuk & B. Czerny astro-ph/0703073: On the neutron star-disc interaction in Be/X-ray binaries by P. Reig astro-ph/0703205: Quasi periodic oscillations in XTE J0111.2–7317, highest frequency among the HMXB pul- sars by Ramanpreet Kaur et al. astro-ph/0703441: Determination of Black Hole Mass in Cyg X-1 by Scaling of Spectral Index-QPO Frequency Correlation by Nickolai Shaposhnikov & Lev Titarchuk astro-ph/0703499: Exploring the connection between the and the non-thermal emission in LS 5039 by V. Bosch-Ramon et al. astro-ph/0704.0452: Dramatic Variability of X-ray Absorption Lines in the Black Hole Candidate Cygnus X-1 by Chulhoon Chang, Wei Cui astro-ph/0704.0536: Binaries, microquasars and GLAST by Guillaume Dubus astro-ph/0704.0543: Swift/XRT observes the fifth outburst of the periodic Supergiant Fast X-ray Transient IGR J11215-5952 by P. Romano et al. astro-ph/0704.0799: Spin Evolution of Accreting Neutron Stars: Nonlinear Development of the R-mode Insta- bility by Ruxandra Bondarescu et al. astro-ph/0704.0811: Jet interactions in massive X-ray binaries by Gustavo E. Romero astro-ph/0704.2192: Comptonization and the Spectra of Accretion-Powered X-Ray Pulsars by Michael T. Wolff et al. astro-ph/0704.2255: Precise Timing of the X-ray Pulsar 1E 1207.4-5209: A Steady Neutron Star Weakly Mag- netized at Birth by E. V. Gotthelf & J. P. Halpern astro-ph/0704.2589: Now you see it, now you don’t - the circumstellar disk in the GRO J1008–57 system by M. J.Coe (Southampton) et al. 4 AS SEENON ASTRO-PH 24 astro-ph/0704.2737: INTEGRAL high energy detection of the transient IGR J11321-5311 by V. Sguera et al. astro-ph/0704.2874: 4U 0115+63 from RXTE and INTEGRAL Data: Pulse Profile and Cyclotron Line En- ergy by S.S. Tsygankov et al. astro-ph/0704.3224: Supergiant Fast X-ray Transients: A common behaviour or a class of objects? by Ignacio Negueruela et al.

4.4 ULXs and extragalactic XRBs astro-ph/0611040: Ultra-luminous X-ray sources: X-ray binaries in a high/hard state? by Z. Kuncic et al. astro-ph/0611152: Recipes for ULX formation: necessary ingredients and garnishments by Roberto Soria astro-ph/0611153: Soft-excess in ULX spectra: the chilled-disk scenario by Roberto Soria, Anabela Goncalves, Zdenka Kuncic astro-ph/0611437: Variability of ultraluminous X-ray sources in the Cartwheel Ring by A. Wolter, G. Trinchieri, M. Colpi astro-ph/0611939: Accretion Disk Spectra of the Brightest Ultra-luminous X-ray Source in M82 by Feng Yuan et al. astro-ph/0612036: Soft-excess in ULX spectra: disc emission or wind absorption? by A. C. Goncalves et al. astro-ph/0612059: Photometric Analysis of the Optical Counterpart of the Black Hole HMXB M33 X-7 by Avi Shporer et al. astro-ph/0612420: X-ray and optical variability of the ultraluminous X-ray source NGC 1313 X-2 by P. Muc- ciarelli et al. astro-ph/0701125: X-Ray Properties of the Point Source Population in the Spiral Galaxy NGC 5055 (M63) with Chandra by Bing Luo et al. astro-ph/0701406: Bright X-ray source populations in the starburst galaxies NGC 4038/4039 by Xi-Wei Liu & Xiang-Dong Li astro-ph/0701764: Irradiation models for ULXs and fits to optical data by C. M. Copperwheat et al. astro-ph/0702274: Constraints on accretion in Ultraluminous X-ray Sources from Spitzer IRS observations of NGC 4485/90: Infrared diagnostic diagrams by Gerardo A. Vazquez et al. astro-ph/0702580: Dynamical Formation of X-ray binaries in the inner bulge of M31 by Rasmus Voss & Marat Gilfanov astro-ph/0702744: Discovery of a Transient X-ray Source in the Compact Stellar Nucleus of NGC 2403 by Mihoko Yukita et al. astro-ph/0703060: Long-term pulse profile study of the Be/X-ray pulsar SAX J2103.5+4545 by A. Camero Arranz et al. astro-ph/0703270: A 33 hour period for the Wolf-Rayet/black hole X-ray binary candidate NGC 300 X-1 by S. Carpano et al. astro-ph/0703697: Optical studies of the ultraluminous X-ray source NGC1313 X-2 by Jifeng Liu et al. astro-ph/0704.1442: On the Nature of Ultra-Luminous X-ray Sources from Optical/IR Measurements by Mark Cropper et al.

4.5 Accretion discs and accretion theory astro-ph/0611010: Relativistic Diskoseismology. III. Low-Frequency Fundamental p-Modes by Manuel Ortega-Rodriguez et al. astro-ph/0612300: Accretion Discs with Strong Toroidal Magnetic Fields by M.C. Begelman & J.E. Pringle astro-ph/astro-ph/0612752: Time-dependent models of two-phase accretion discs around black holes by M. Mayer & J.E. Pringle astro-ph/0612752: Flickering in Black Hole Accretion discs by M. Mayer & J.E. Pringle astro-ph/0701035: Accretion disc dynamics in extreme mass ratio compact binaries by Michael Truss 4 AS SEENON ASTRO-PH 25 astro-ph/0701272: 3D Relativistic MHD Simulation of a Tilted Accretion Disk Around a Rapidly Rotating Black Hole by P. Chris Fragile et al. astro-ph/0702185: A Note on the Slim Accretion Disk Model by Wei-Min Gu & Ju-Fu Lu astro-ph/0703301: Evolution of transonicity in an accretion disc by Arnab K. Ray, Jayanta K. Bhattacharjee astro-ph/0704.0467: Modeling Accretion Disk X-ray Continuum of Black Hole Candidates by Gabor Pszota & Wei Cui astro-ph/0704.1519: Comprehensive simulations of superhumps by Amanda J. Smith et al. astro-ph/0704.1920: Global Disk Oscillation Modes in Cataclysmic Variables and Other Newtonian Accre- tors by Manuel Ortega-Rodriguez & Robert V. Wagoner astro-ph/0704.2159: Accretion Disk Illumination in Schwarzschild and Kerr Geometries: Fitting Formulae by Keigo Fukumura & Demosthenes Kazanas astro-ph/0704.2643: Eclipsing light curves for accretion flows around a rotating black hole and atmospheric effects of the companion star by Rohta Takahashi & Ken-Ya Watarai astro-ph/0704.3394: Modelling the energy dependencies of high-frequency QPO in black hole X-ray bina- ries by P. T. Zycki et al.

4.6 Mergers, SNIa, and accretion induced collapse astro-ph/0611009: Capturing the Fire: Flame Energetics and Neutronizaton for Type Ia Supernova Simula- tions by A. C. Calder et al. astro-ph/0704.0297: Remnant evolution after a carbon-oxygen white dwarf merger by Sung-Chul Yoon et al. astro-ph/0611047: Relativistic neutron star merger simulations with non-zero temperature equations of state I. Variation of binary parameters and equation of state by R. Oechslin, H.-T. Janka, A. Marek astro-ph/0611522: Merger of black hole-neutron star binaries in full general relativity by Masaru Shibata, Koji Uryu astro-ph/0612015: Remnants of compact binary mergers by W. Domainko & M. Ruffert astro-ph/0612032: On the rarity of double black hole binaries: consequences for gravitational-wave detec- tion by Krzysztof Belczynski et al. astro-ph/0612055: Compact Binaries as Sources of Gravitational Radiation by M. Coleman Miller astro-ph/0612144: Formation of Double Compact Objects by V. Kalogera et al. astro-ph/0612572: Last moments in the life of a compact binary system: gravitational waves, gamma-ray bursts and formation by S. Rosswog astro-ph/0701004: Stochastic background from inspiralling double neutron stars by Tania Regimbau astro-ph/0702390: Modeling kicks from the merger of non-precessing black-hole binaries by John G. Baker et al. astro-ph/0703292: Astrophysics of white dwarf binaries by G. Nelemans astro-ph/0703415: Progenitors of Type Ia Supernovae: Binary Stars with White Dwarf Companions by M. Parthasarathy et al. astro-ph/0703599: Mergers of Black Hole – Neutron Star binaries. I. Methods and First Results by Em- manouela Rantsiou et al. astro-ph/0704.1215: Double Neutron Stars: Evidence For Two Different Neutron- Mecha- nisms by E.P.J. van den Heuvel astro-ph/0704.1258: Evidence for a merger of binary white dwarfs: the case of GD 362 by E. Garcia-Berro, P. Loren-Aguilar, A.G. Pedemonte, J. Isern, P. Bergeron, P. Dufour, P. Brassard

4.7 Radio pulsars in binaries (and otherwise) astro-ph/0611022: What can the braking indices tell us about pulsars’ nature? by Y. L. Yue, R. X. Xu, W. W. Zhu astro-ph/0611041: “High-field” pulsars torqued by accretion disk? by Y. L. Yue, W. W. Zhu, R. X. Xu 4 AS SEENON ASTRO-PH 26 astro-ph/0611068: The Origin and Motion of PSR J0538+2817 in S147 by C.-Y. Ng et al. astro-ph/0611082: A search for radio pulsars around low-mass white dwarfs by Joeri van Leeuwen et al. astro-ph/0611222: Timing an Accreting Millisecond Pulsar: Measuring the Accretion Torque in IGR J00291+5934 by L. Burderi et al. astro-ph/0611309: Production and evolution of millisecond X-ray and radio pulsars by Frederick K. Lamb astro-ph/0611320: Be born slow or die fast: spin evolution of neutron stars with alignment or counteralign- ment by S.A. Eliseeva, S.B. Popov, V.S. Beskin astro-ph/0611398: Binary and recycled pulsars: 30 years after observational discovery by G S Bisnovatyi- Kogan astro-ph/0611436: The PSR J1811-1736: evidence of a low amplitude supernova kick by A.Corongiu et al. astro-ph/0611551: Emission of gravitational waves from binary systems in the galactic center and diffraction by star clusters by P. Longo et al. astro-ph/0611680: Pulsar spins from an instability in the accretion shock of supernovae by John M. Blondin, Anthony Mezzacappa astro-ph/0611729: PSR B1828-11: a precession pulsar torqued by a quark ? by K. Li, Y. L. Yue, R. X. Xu astro-ph/0611942: Timing of the Accreting Millisecond Pulsar XTE J1814-338 by A.Papitto et al. astro-ph/0701059: The Evolution of Compact Binary Star Systems by Konstantin Postnov et al. astro-ph/0701097: Finding binary millisecond pulsars with the Hough transform by C. Aulbert astro-ph/0701183: The 8gr8 Cygnus survey for new pulsars and RRATs by E. Rubio-Herrera et al. astro-ph/0701290: Detailed studies of giant pulses from the millisecond pulsar B1937+21 by V.I. Kondratiev et al. astro-ph/0701296: INTEGRAL observations of PSR B0540-69 by A. Slowikowska et al. astro-ph/0701444: The birth properties of Galactic millisecond radio pulsars by Lilia Ferrario & Dayal Wick- ramasinghe astro-ph/0702347: The Unusual Binary Pulsar PSR J1744-3922: Radio Flux Variability, Near-infrared Obser- vation and Evolution by R. P. Breton et al. astro-ph/0702540: Binary star progenitors of long gamma-ray bursts by M. Cantiello et al. astro-ph/0702698: Curious properties of the recycled pulsars and the potential of high precision timing by Matthew Bailes astro-ph/0703181: Pulsed X-ray Emission from Pulsar A in the Double Pulsar System J0737-3039 by S. Chat- terjee et al. astro-ph/0703239: The blast wave of Tycho’s supernova remnant by Gamil Cassam-Chenai et al. astro-ph/0704.0973: X-ray Timing Observations of PSR J1930+1852 in the Crab-like SNR G54.1+0.3 by Fangjun Lu et al. astro-ph/0704.2079: X-ray emission from the planet pulsar B1257+12 by G. G. Pavlov et al.

4.8 Magnetars: AXPs and SGRs astro-ph/0611100: Spitzer Mid-infrared Upper Limits on Anomalous X-Ray Pulsars 1E 1048.1-5937, 1RXS J170849-400910, and XTE J1810-197 by Z. Wang, V. M. Kaspi, S. J. U. Higdon astro-ph/0611175: The first multi-wavelength campaign of AXP 4U 0142+61 from radio to hard X-rays by P.R. den Hartog et al. astro-ph/0611216: Swift and Chandra confirm the intensity-hardness correlationof the AXP 1RXS J170849.0- 400910 by S. Campana et al. astro-ph/0611368: Assessing Millisecond Proto-Magnetars as GRB Central Engines by Todd A. Thompson astro-ph/0611405: Inferring the Magnetic Fields of Magnetars from their X-ray Spectra by Tolga Guver, Feryal Ozel, Maxim Lyutikov 4 AS SEENON ASTRO-PH 27 astro-ph/0611442: The origin of long-period X-ray pulsars by N.R. Ikhsanov astro-ph/0611608: AXPs/SGRs: Magnetars or Quark-stars? by Renxin Xu astro-ph/0611747: Long Term Cooling of Magnetar Crusts by David Eichler et al. astro-ph/0611752: Search for optical activity of SGR 1806-20 by G. Beskin et al. astro-ph/0611810: Multi-wavelength variability of the magnetar 4U 0142+61 by Martin Durant, Marten H. van Kerkwijk astro-ph/0611860: SGRs in nearby galaxies: rate, luminosity function and fraction among short GRBs by Eran O. Ofek astro-ph/0612252: Neutron star oscillations and QPOs during magnetar flares by Anna L. Watts & Tod E. Strohmayer astro-ph/0612289: Giant Flare in SGR 1806-20 and Its Compton Reflection from the by D.D.Frederiks et al. astro-ph/0612319: Solving GRBs and SGRs puzzles by precessing Jets by D.Fargion et al. astro-ph/0612437: IGR J08408–4503: a new recurrent Supergiant Fast X-ray Transient by D. Gotz, M. Falanga, F. Senziani, A. De Luca, S. Schanne, A. von Kienlin astro-ph/0612587: Anomalous X-ray pulsars: Persistent States with Fallback Disks by Unal Ertan et al. astro-ph/0702598: SGR1806-20: evidence for a superstrong Magnetic Field from Quasi Periodic Oscilla- tions by M. Vietri et al. astro-ph/0703128: Spectral modelling of the high energy emission of the magnetar 4U 0142+614 by Nanda Rea et al. astro-ph/0703246: Deep Searches for Radio Pulsations and Bursts from Four Southern Anomalous X-ray Pulsars by Fronefield Crawford et al. astro-ph/0703684: The Post-Burst Awakening of the Anomalous X-ray Pulsar in Westerlund 1 by G.L. Israel et al.

4.9 Other binary systems astro-ph/0704.0059: The Mass and Radius of the Unseen M-Dwarf Companion in the Single-Lined Eclipsing Binary HAT-TR-205-013 by T. G. Beatty et al. astro-ph/0704.0387: Low mass visual binaries in the solar neighbourhood: The case of HD141272 by T. Eisen- beiss et al. astro-ph/0611088: Winds in Collision: high-energy particles in massive binary systems by Sean M. Dougherty, Julian M. Pittard astro-ph/0611482: Analysis of the eclipsing binaries in the LMC discovered by OGLE: Period distribution and frequency of the short-period binaries by Tsevi Mazeh, Omer Tamuz, Pierre North astro-ph/0611505: Binaries and the L Dwarf/T Dwarf Transition by Adam J. Burgasser astro-ph/0611616: Improved age constraints for the AB Dor quadruple system - The binary nature of AB Dor B by Markus Janson et al. astro-ph/0611636: A Survey for Young Spectroscopic Binary K7-M4 Stars in Ophiuchus by L. Prato astro-ph/0611647: Gamma rays from colliding winds of massive stars by Anita Reimer, Olaf Reimer, Martin Pohl astro-ph/0611656: Eclipsing binaries in the LMC: a wealth of data for astrophysical tests by A. Derekas, L. L. Kiss, T. R. Bedding astro-ph/0611662: Eclipsing Binaries in Open Clusters by John Southworth astro-ph/0611697: Discovery of a High Proper Motion L Dwarf Binary: 2MASS J15200224-4422419AB by Adam J. Burgasser et al. astro-ph/0611822: Mass Transfer in Close, Rapidly Accreting Protobinaries: An Origin for Massive Twins? by Mark R. Krumholz, Todd A. Thompson 4 AS SEENON ASTRO-PH 28 astro-ph/0611855: Determination of Mass Loss and Mass Transfer Rates of Algol (Beta Persei) from the Anal- ysis of Absorption Lines in the UV Spectra Obtained by the IUE Satellite by Kristen Wecht astro-ph/0611875: Radial Velocity Studies of Close Binary Stars. XII by Theodor Pribulla et al. astro-ph/0612138: Precision Masses of the low-mass binary system GJ 623 by Frantz Martinache et al. astro-ph/0612161: Spitzer Observations of the New M85OT2006-1 by A. Rau et al. astro-ph/0612234: The widest ultracool binary by Jose A. Caballero astro-ph/0612438: Binary life after the AGB - towards a unified picture by A. Frankowski & A. Jorissen astro-ph/0612477: Massive binaries, Wolf-Rayet stars and supernova progenitors by J.J. Eldridge astro-ph/0612539: On Rejuvenation in Massive Binary Systems by L. M. Dray & C. A. Tout astro-ph/0701080: Investigating Binary Properties with Next-Generation Microlensing Surveys by Cheongho Han astro-ph/0701200: Physical parameters and multiplicity of five southern close eclipsing binaries by T. Szalai et al. astro-ph/0701459: Asteroseismology of close binary stars by Conny Aerts astro-ph/0702013: Discovery of a 66 mas Ultracool Binary with Laser Guide Star Adaptive Optics by Nick Siegler et al. astro-ph/0702171: Late-Type Near-Contact Eclipsing Binary [HH97] FS Aur-79 by S. J. Austin et al. astro-ph/0702631: New periodic variable stars coincident with ROSAT sources discovered using Super- WASP by A.J. Norton et al. astro-ph/0702647: Discovery of the Widest Very Low Mass Binary by Etienne Artigau et al. astro-ph/0702658: Eclipsing Binary System WN3(h)+O5V BAT99-129: Analysis of the MACHO Light Curve and the Parameters of the Components by I. I. Antokhin & A. M. Cherepashchuk astro-ph/0703061: LP133-373: A New Chromospherically Active Eclipsing dMe Binary with a Distant, Cool White Dwarf Companion by T.R. Vaccaro et al. astro-ph/0703137: Eclipsing binaries in the MACHO database: New periods and classifications for 3031 sys- tems in the Large Magellanic Cloud by A. Derekas et al. astro-ph/0703579: A new detached K7 dwarf eclipsing binary system by T.B. Young et al. astro-ph/0703614: Pulsating components of eclipsing binaries in the ASAS-3 catalog by A. Pigulski & G. Michalska astro-ph/0703634: Eclipsing binaries observed with the WIRE satellite. II. beta Aurigae and non-linear limb darkening in light curves by John Southworth et al. astro-ph/0703693: Contact binaries with additional components. III. The adaptive optics detections by Slavek M. Rucinski et al. astro-ph/0703705: ASAS Eclipsing Binaries with Observed High Period Change Rates by B. Pilecki et al. astro-ph/0704.2469: The young, wide and very low mass visual binary LOri167 by D. Barrado y Navascues et al. astro-ph/0704.3106: A Surprising Reversal of Temperatures in the Brown-Dwarf Eclipsing Binary 2MASS J05352184-0546085 by Keivan G. Stassun et al. astro-ph/0704.3229: The Long Period, Massive Binaries HD 37366 and HD 54662: Potential Targets for Long Baseline Optical Interferometry by T. S. Boyajian et al.