List of Publications1

Total Page:16

File Type:pdf, Size:1020Kb

List of Publications1 List of Publications1 Vassiliki (Vicky) Kalogera [h-indices from NASA ADS system: 71 (34,100+ citations) without and 97 (50,500+ citations) with the \Other LIGO Scientific Collaboration publications", respectively] Before 1998: 1. On the Origin of Low-Mass X-Ray Binaries Webbink, R. F. & Kalogera, V. 1994, in The Evolution of X-Ray Binaries, ed. S. S. Holt & C. S. Day (New York: American Institute of Physics Conf. Proc. No. 308), p. 321{330 2. • Formation of Low-Mass X-Ray Binaries. I. Constraints on Hydrogen-Rich Donors at the Onset of the X-Ray Phase Kalogera, V. & Webbink, R. F. 1996, The Astrophysical Journal, 458, 301{311 3. • A Strongly Magnetic Neutron Star in a Face-On Binary System Daumerie, P., Kalogera, V., Lamb, F. K., & Psaltis, D. 1996, Nature, 382, 141{144 4. • The Maximum Mass of a Neutron Star Kalogera, V. & Baym G. 1996, The Astrophysical Journal Letters, 470, L61{64 5. • Orbital Characteristics of Binary Systems after Asymmetric Supernova Explosions Kalogera, V. 1996, The Astrophysical Journal, 471, 352{365 6. A New Mechanism for the Formation of LMXBs: Direct Supernova Kalogera, V. 1996, in the Proceedings of the 2nd Hellenic Astronomical Conference, ed. M. E. Contadakis, J. D. Hadjidemetriou, L. N. Mavridis, & J. H. Seiradakis (Thessaloniki: Hellenic Astronomical Society), p. 335{340 7. • Double Neutron Star Systems and Natal Neutron Star Kicks Fryer, C. L. & Kalogera, V. 1997, The Astrophysical Journal, 489, 244{253 8. Super-Eddington Accretion in the Formation of Low-Mass X-ray Binaries and Millisecond Pulsars Webbink, R. F. & Kalogera, V. 1997, in Accretion Phenomena and Related Outflows, IAU Col- loquium 163, ed. D. T. Wickramasinghe, L. Ferrario, & G. V. Bicknell (San Francisco: ASP Conf. Ser., Vol. 121), p. 828{829 In 1998: 9. • Formation of Low-Mass X-Ray Binaries. II. Common Envelope Evolution of Primordial Binaries with Extreme Mass Ratios Kalogera, V. & Webbink, R. F. 1998, The Astrophysical Journal, 493, 351{367 10. • Formation of Low-Mass X-Ray Binaries. III. A New Formation Mechanism: Direct Supernova Kalogera, V. 1998, The Astrophysical Journal, 493, 368{374 11. • Supernova Kicks, Magnetic Braking, and Neutron-Star Binaries Kalogera, V., Kolb, U., & King, A. R. 1998, The Astrophysical Journal, 504, 967{977 12. Kinematics of Low-Mass X-ray Binaries and Millisecond Pulsars Kalogera, V. 1998, in Pulsars and Neutron Stars, ed. N. Shibazaki, N. Kawai, S. Shibata, & T. Kifune (Tokyo: Universal Academy Press), p. 27{30 13. The Effect of Kick Velocities on the Formation of Low-Mass X-ray Binaries Kalogera, V. 1998, in The Many Faces of Neutron Stars, ed. R. Buccheri, J. van Paradijs, & M. A. Alpar (Dordrecht: Kluwer Academic Publishers), p. 505{511 1Publications in Peer-Reviewed Journals marked with • 1 In 1999: 14. • Donor Stars in Black-Hole X-Ray Binaries Kalogera, V. 1999, The Astrophysical Journal, 521, 723{734 15. Coalescence Rates of Double Neutron Stars Kalogera, V. 1999, Gravitational Waves and Experimental Gravity, 1999 Rencontres de Moriond, ed. P. Demarchez, p. 343{348 16. • Formation of the Observed Double Neutron Star Systems Kalogera, V. & Fryer, C. L. 1999, The Astrophysical and Astronomical Transactions, 18, p. 515{ 520 (Refereed proceedings of the 4th JENAM) In 2000: 17. • Bounds on Neutron-Star Moments of Inertia and the Evidence for General Relativistic Frame Dragging Kalogera, V. & Psaltis, D. 2000, Physical Review D, Vol. 61, id.024009 18. Close Binaries with Two Compact Objects Kalogera, V. 2000, in Pulsar Astronomy - 2000 and Beyond, IAU Colloquium No. 177, ed. M. Kramer, N. Wex, and R. Wielebinski (San Francisco: ASP Conf. Ser., Vol. 202), p. 579{584 19. Compact Binary Mergers and Accretion-Induced Collapse: Event Rates Kalogera, V. 2000, in the proceedings of the Third Edoardo Amaldi Conference on Gravitational Waves, ed. S. Meshkov, p. 41{50 20. • Constraints on Supernova Kicks from the Double Neutron Star System PSR B1913+16 Wex, N., Kalogera, V., & Kramer, M. 2000, The Astrophysical Journal, 528, 401{409 21. • An Upper Limit on the Coalescence Rate of Double Neutron-Star Binaries in the Galaxy Kalogera, V. & Lorimer, D. R. 2000, The Astrophysical Journal, 530, 890{895 22. • Spin-Orbit Misalignment in Close Binaries with Two Compact Objects, Kalogera, V. 2000, The Astrophysical Journal, 541, 319{328 23. Chandra Observations of M33: A First Look McDowell, J.C., Fabbiano, G., Kalogera, V., Stanek, K., & Sasselov, D. 2000, in The Interstellar Medium in M31 and M33, WE-Heraeus Seminar, eds. E.M. Berkhuijsen and R. Beck, p. 153{154 In 2001: 24. Coalescence Rates of Compact Objects Kalogera, V. 2001, in The Neutron Star - Black Hole Connection, eds. J. Ventura, C. Kouveliotou, J. van Paradijs, p. 89{94 25. Asymmetric Supernova Explosion Investigated by Geodetic Precession Kramer, M., Wex, N., Kalogera, V., & Karastergiou, A. 2001, in Galaxies and their Constituents at the Highest Angular Resolution, IAU Symposium 205 (San Francisco: ASP Conf. Ser.), ed. R. Schilizzi, p. 410{411 26. Formation of Black-Hole X-Ray Binaries with Low-Mass Donors Kalogera, V. 2001, in Black Holes in Binaries and Galactic Nuclei, ESO Workshop in Honour of Prof. R. Giacconi, eds. L. Kaper, E. P. J. van den Heuvel, & P. A. Woudt, p. 299{304 27. Formation of Black-Hole X-Ray Transients Kalogera, V. 2001, in Evolution of Binary and Multiple Stars, Meeting in Celebration of P.P Eggleton's 60th Birthday, eds . P. Podsiadlowski, S. Rappaport, A.R. King, F. D'Antona & L. Burderi (San Francisco: ASP Conf. Ser.), p. 537{546 2 28. • A New Formation Channel for Double Neutron Stars Without Recycling: Implications for Grav- itational Wave Detection Belczynski, K., & Kalogera, V. 2001, The Astrophysical Journal Letters, 550, L183{187 29. • Theoretical Black Hole Mass Distributions Fryer, C. L. & Kalogera, V., 2001, The Astrophysical Journal, 554, 548{560 30. • The Coalescence Rate of Double Neutron Star Systems Kalogera, V., Narayan, R., Spergel, D., & Taylor, J.H. 2001, The Astrophysical Journal, 556, 340{356 31. Event Rates for Binary Inspiral Kalogera, V. 2001, in Workshop on Astrophysical Sources for Ground-Based Gravitational Wave Detectors, ed. J. Centrella, p. 107{118 32. Binary Population Synthesis: Methods, Normalization, and Surprises Kalogera, V., & Belczynski, K. 2001, in The Influence of Binaries on Stellar Population Studies, ed. D. Vanbeveren (Kluwer Academic Publishers), p. 447{461 In 2002: 33. Coalescence of Double Compact Objects: Event Rates Kalogera, V. 2002, in Stellar Collisions, Mergers, and Their Consequences, ed. M. Shara, (San Francisco: ASP Conf. Ser.), p. 323{331 34. • Merger Sites of Double Neutron Stars and Their Host Galaxies Belczynski, K., Bulik, T., & Kalogera, V. 2002, The Astrophysical Journal Letters, 571, L147{ L150 35. • A Comprehensive Study of Binary Compact Objects as Gravitational Wave Sources: Evolutionary Channels, Rates, and Physical Properties Belczynski, K. Kalogera, V., & Bulik, T. 2002, The Astrophysical Journal, 572, 407{431 In 2003: 36. A New Method for Estimates of Binary Pulsar Coalescence Rates Kalogera, V., Kim, C.-L., & Lorimer, D.R. 2003, in Astronomical Telescopes and Instrumentation: Astronomy Outside the EM Spectrum, p. 134{145 37. Influence of Precession on the Search of Inspiral Binaries with Ground-Based Gravitational-Wave Detectors Grandcl´ement, P., Kalogera, V., & Vecchio, A. 2003, in Astronomical Telescopes and Instrumen- tation: Astronomy Outside the EM Spectrum, p. 167{176 38. The Distribution of Mass Ratios in Compact Object Binaries Bulik, T., Belczynski, K., & Kalogera, V. 2003, in Astronomical Telescopes and Instrumentation: Astronomy Outside the EM Spectrum, p. 146{155 39. • Searching for Gravitational Waves from the Inspiral of Precessing Binary Systems: Problems with Current Waveforms Grandcl´ement, P., Kalogera, V., & Vecchio, A. 2003, Physical Review D, 67, 042003{042008 40. The Probability Distribution of the Double Neutron Star Coalescence Rate and Predictions for More Detections Kalogera, V., Kim, C., & Lorimer, D.R. 2003, in Radio Pulsars (ASP Conf. Ser.), eds. M.Bailes, D.Nice, & S. Thorsett, p. 299{306 41. • The Probability Distribution of Binary Pulsar Coalescence Rates. I. Double Neutron Star Systems in the Galactic Field Kim, C.-L., Kalogera, V., & Lorimer, D.R. 2003, The Astrophysical Journal, 584, 985{995 3 42. • Searching for Gravitational Waves from the Inspiral of Precessing Binary Systems: New Hierar- chical Scheme using \Spiky" Templates Grandcl´ement, P. & Kalogera, V. 2003, Physical Review D, 67, 082002-082013 43. • Helium-Core White Dwarfs in Globular Clusters Hansen, B., Kalogera, V., & Rasio, F. 2003, The Astrophysical Journal, 586, 1364{1373 44. • The Role of Helium Stars in the Formation of Double Neutron Stars Ivanova, N., Belczynski, K., Kalogera, V., Rasio, F., & Taam, R.E. 2003, The Astrophysical Journal, 592, 475{485 45. The Probability Distribution of Binary Pulsar Coalescence Rates Kim, C., Kalogera, V., & Lorimer, D.R. 2003, in The Astrophysics of Gravitational Wave Sources, ed. J.M.Centrella, 686, p. 281{284 46. • An Increased Estimate of the Merger Rate of Double Neutron Stars from Observations of a Highly Relativistic System Burgay, M., et al., Kalogera, V., Kim, C., & Lorimer, D.R. 2003, Nature, 426, 531{533 47. First Results from a Chandra Survey of the 'Bar' Region of the SMC Zezas, A., McDowell, J. C., Hadzidimitriou, D., Kalogera, V.; Fabbiano, G., & Taylor, P. 2003, in The Local Group as an Astrophysical Laboratory, ed. M.Livio & T.M. Brown, p. 111{112 In 2004: 48. • X-Ray Binary Populations: The Luminosity Function of NGC 1569 Belczynski, K., Kalogera, V., Zezas, A., & Fabbiano, G. 2004, The Astrophysical Journal Letters, 601, L147-L150 49. • Could Black Hole X-ray Binaries be Detected in Globular Clusters? Kalogera, V., King, A.R., & Rasio, F.A. 2004, The Astrophysical Journal Letters, 601, 2, L171{ L174 50. • The Cosmic Coalescence Rate for Double Neutron Star Binaries Kalogera, V., Kim, C., Lorimer, D.R., Burgay, M., et al.
Recommended publications
  • Gnc 2021 Abstract Book
    GNC 2021 ABSTRACT BOOK Contents GNC Posters ................................................................................................................................................... 7 Poster 01: A Software Defined Radio Galileo and GPS SW receiver for real-time on-board Navigation for space missions ................................................................................................................................................. 7 Poster 02: JUICE Navigation camera design .................................................................................................... 9 Poster 03: PRESENTATION AND PERFORMANCES OF MULTI-CONSTELLATION GNSS ORBITAL NAVIGATION LIBRARY BOLERO ........................................................................................................................................... 10 Poster 05: EROSS Project - GNC architecture design for autonomous robotic On-Orbit Servicing .............. 12 Poster 06: Performance assessment of a multispectral sensor for relative navigation ............................... 14 Poster 07: Validation of Astrix 1090A IMU for interplanetary and landing missions ................................... 16 Poster 08: High Performance Control System Architecture with an Output Regulation Theory-based Controller and Two-Stage Optimal Observer for the Fine Pointing of Large Scientific Satellites ................. 18 Poster 09: Development of High-Precision GPSR Applicable to GEO and GTO-to-GEO Transfer ................. 20 Poster 10: P4COM: ESA Pointing Error Engineering
    [Show full text]
  • GW170104: Observation of a 50-Solar-Mass Binary Black Hole Coalescence at Redshift 0.2 – Supplemental Material
    GW170104: Observation of a 50-Solar-Mass Binary Black Hole Coalescence at Redshift 0.2 { Supplemental Material The LIGO Scientific Collaboration and the Virgo Collaboration I. NOISE PERFORMANCE OF THE sis used an initial calibration of the data and assumed DETECTORS a (conservative) one-sigma calibration uncertainty of 10% in amplitude and 10◦ in phase for both detec- Figure 1 shows a comparison of typical strain noise am- tors, a reduced-order quadrature model of the effective- plitude spectra during the first observing run and early precession waveform [15{18] (the most computationally in the second for both of the LIGO detectors [1]. For the expedient model), and a power spectral density cal- Hanford detector, shot-noise limited performance was im- culated using a parametrized model of the detector proved above about 500 Hz by increasing the laser power. noise [19, 20]. A stretch of 4 s of data, centered on There are new broad mechanical resonance features (e.g., the event, was analysed across a frequency range of 20{ at 150 Hz, 320 Hz and 350 Hz) due to increased beam 1024 Hz. We assumed uninformative prior probabili- pointing∼ jitter from the laser, as well as the coupling ties [11, 13]; technical restrictions of the reduced-order of the jitter to the detector's gravitational-wave channel quadrature required us to limit spin magnitudes to < 0:8 that is larger than in the Livingston detector. The in- and impose cuts on the masses (as measured in the de- det det crease in the noise between 40 Hz and 100 Hz is currently tector frame) such that m1;2 [5:5; 160] M , 2 M 2 under investigation.
    [Show full text]
  • Determining the Hubble Constant with Black Hole Mergers in Active Galactic Nuclei
    Determining the Hubble Constant with AGN-assisted Black Hole Mergers Y. Yang,1 V. Gayathri,1 S. M´arka,2 Z. M´arka,2 and I. Bartos1, ∗ 1Department of Physics, University of Florida, PO Box 118440, Gainesville, FL 32611, USA 2Department of Physics, Columbia University in the City of New York, New York, NY 10027, USA Gravitational waves from neutron star mergers have long been considered a promising way to mea- sure the Hubble constant, H0, which describes the local expansion rate of the Universe. While black hole mergers are more abundantly observed, their expected lack of electromagnetic emission and poor gravitational-wave localization makes them less suited for measuring H0. Black hole mergers within the disks of Active Galactic Nuclei (AGN) could be an exception. Accretion from the AGN disk may produce an electromagnetic signal, pointing observers to the host galaxy. Alternatively, the low number density of AGNs could help identify the host galaxy of 1 − 5% of mergers. Here we show that black hole mergers in AGN disks may be the most sensitive way to determine H0 with gravitational waves. If 1% of LIGO/Virgo's observations occur in AGN disks with identified host galaxies, we could measure H0 with 1% uncertainty within five years, likely beyond the sensitivity of neutrons star mergers. I. INTRODUCTION Multi-messenger gravitational-wave observations rep- resent a valuable, independent probe of the expansion of the Universe [1]. The Hubble constant, which de- scribes the rate of expansion, can measured using Type Ia supernovae, giving a local expansion rate of H0 = 74:03 ± 1:42 km s−1 Mpc−1 [2].
    [Show full text]
  • Continuous Gravitational Waves from Neutron Stars: Current Status and Prospects
    Continuous gravitational waves from neutron stars: current status and prospects Magdalena Sieniawska∗1 and Michał Bejger1 1Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, Bartycka 18, 00–716 Warszawa, Poland Abstract Gravitational waves astronomy allows us to study objects and events invisi- ble in electromagnetic waves. It is crucial to validate the theories and models of the most mysterious and extreme matter in the Universe: the neutron stars. In addition to inspirals and mergers of neutrons stars, there are currently a few pro- posed mechanisms that can trigger radiation of long-lasting gravitational radiation from neutron stars, such as e.g., elastically and/or magnetically driven deforma- tions: mountains on the stellar surface supported by the elastic strain or magnetic field, free precession, or unstable oscillation modes (e.g., the r-modes). The as- trophysical motivation for continuous gravitational waves searches, current LIGO and Virgo strategies of data analysis and prospects are reviewed in this work. 1 Introduction Gravitational-wave (GW) astronomy has been one of the fastest-growing fields in astro- physics since the first historical detection of a binary black-hole (BH) system GW150814 (Abbott et al., 2016a). In addition to studying the nature of gravitation itself, it may be used to infer information about the astrophysical sources emitting the GWs. This re- view concentrates on a specific kind of prospective GWs: persistent (continuous) grav- itational waves (CGWs), emitted by neutron stars (NSs). The article is arranged as follows. Section1 gathers introductory material: Section 1.1 presents the basics of the GWs theory, Section 1.2 contains a brief overview of GWs detections, Section 1.3 de- arXiv:1909.12600v2 [astro-ph.HE] 5 Nov 2019 scribes properties of NSs and features of hitherto detected NSs-related GWs—a binary NS merger GW170817 (Abbott et al., 2017d), Section 1.4 gathers general information about CGWs, whereas Section 1.5 is devoted to the main data analysis methods used in CGWs searches.
    [Show full text]
  • Search for Electron-Antineutrinos Associated with Gravitational-Wave Events GW150914, GW151012, GW151226, GW170104, GW170608, GW170814, and GW170817 at Daya Bay*
    Chinese Physics C Vol. 45, No. 5 (2021) 055001 Editors′ Suggestion Search for electron-antineutrinos associated with gravitational-wave events GW150914, GW151012, GW151226, GW170104, GW170608, GW170814, and GW170817 at Daya Bay* F. P. An1 A. B. Balantekin2 H. R. Band3 M. Bishai4 S. Blyth5 G. F. Cao6 J. Cao6 J. F. Chang6 Y. Chang7 H. S. Chen6 S. M. Chen8 Y. Chen9,10 Y. X. Chen11 J. Cheng6 Z. K. Cheng10 J. J. Cherwinka2 M. C. Chu12 J. P. Cummings13 O. Dalager14 F. S. Deng15 Y. Y. Ding6 M. V. Diwan4 T. Dohnal16 J. Dove17 M. Dvořák16 D. A. Dwyer18 J. P. Gallo19 M. Gonchar20 G. H. Gong8 H. Gong8 W. Q. Gu4 J. Y. Guo10 L. Guo8 X. H. Guo21 Y. H. Guo22 Z. Guo8 R. W. Hackenburg4 S. Hans4,* M. He6 K. M. Heeger3 Y. K. Heng6 A. Higuera23 Y. K. Hor10 Y. B. Hsiung5 B. Z. Hu5 J. R. Hu6 T. Hu6 Z. J. Hu10 H. X. Huang24 X. T. Huang25 Y. B. Huang26 P. Huber27 D. E. Jaffe4 K. L. Jen28 X. L. Ji6 X. P. Ji4 R. A. Johnson29 D. Jones30 L. Kang31 S. H. Kettell4 S. Kohn32 M. Kramer18,32 T. J. Langford3 J. Lee18 J. H. C. Lee33 R. T. Lei31 R. Leitner16 J. K. C. Leung33 F. Li6 J. J. Li8 Q. J. Li6 S. Li31 S. C. Li27 W. D. Li6 X. N. Li6 X. Q. Li34 Y. F. Li6 Z. B. Li10 H. Liang15 C. J. Lin18 G. L. Lin28 S. Lin31 J. J. Ling10 J. M. Link27 L. Littenberg4 B.
    [Show full text]
  • GW190814: Gravitational Waves from the Coalescence of a 23 M Black Hole 4 with a 2.6 M Compact Object
    1 Draft version May 21, 2020 2 Typeset using LATEX twocolumn style in AASTeX63 3 GW190814: Gravitational Waves from the Coalescence of a 23 M Black Hole 4 with a 2.6 M Compact Object 5 LIGO Scientific Collaboration and Virgo Collaboration 6 7 (Dated: May 21, 2020) 8 ABSTRACT 9 We report the observation of a compact binary coalescence involving a 22.2 { 24.3 M black hole and 10 a compact object with a mass of 2.50 { 2.67 M (all measurements quoted at the 90% credible level). 11 The gravitational-wave signal, GW190814, was observed during LIGO's and Virgo's third observing 12 run on August 14, 2019 at 21:10:39 UTC and has a signal-to-noise ratio of 25 in the three-detector 2 +41 13 network. The source was localized to 18.5 deg at a distance of 241−45 Mpc; no electromagnetic 14 counterpart has been confirmed to date. The source has the most unequal mass ratio yet measured +0:008 15 with gravitational waves, 0:112−0:009, and its secondary component is either the lightest black hole 16 or the heaviest neutron star ever discovered in a double compact-object system. The dimensionless 17 spin of the primary black hole is tightly constrained to 0:07. Tests of general relativity reveal no ≤ 18 measurable deviations from the theory, and its prediction of higher-multipole emission is confirmed at −3 −1 19 high confidence. We estimate a merger rate density of 1{23 Gpc yr for the new class of binary 20 coalescence sources that GW190814 represents.
    [Show full text]
  • Advanced Virgo: Status of the Detector, Latest Results and Future Prospects
    universe Review Advanced Virgo: Status of the Detector, Latest Results and Future Prospects Diego Bersanetti 1,* , Barbara Patricelli 2,3 , Ornella Juliana Piccinni 4 , Francesco Piergiovanni 5,6 , Francesco Salemi 7,8 and Valeria Sequino 9,10 1 INFN, Sezione di Genova, I-16146 Genova, Italy 2 European Gravitational Observatory (EGO), Cascina, I-56021 Pisa, Italy; [email protected] 3 INFN, Sezione di Pisa, I-56127 Pisa, Italy 4 INFN, Sezione di Roma, I-00185 Roma, Italy; [email protected] 5 Dipartimento di Scienze Pure e Applicate, Università di Urbino, I-61029 Urbino, Italy; [email protected] 6 INFN, Sezione di Firenze, I-50019 Sesto Fiorentino, Italy 7 Dipartimento di Fisica, Università di Trento, Povo, I-38123 Trento, Italy; [email protected] 8 INFN, TIFPA, Povo, I-38123 Trento, Italy 9 Dipartimento di Fisica “E. Pancini”, Università di Napoli “Federico II”, Complesso Universitario di Monte S. Angelo, I-80126 Napoli, Italy; [email protected] 10 INFN, Sezione di Napoli, Complesso Universitario di Monte S. Angelo, I-80126 Napoli, Italy * Correspondence: [email protected] Abstract: The Virgo detector, based at the EGO (European Gravitational Observatory) and located in Cascina (Pisa), played a significant role in the development of the gravitational-wave astronomy. From its first scientific run in 2007, the Virgo detector has constantly been upgraded over the years; since 2017, with the Advanced Virgo project, the detector reached a high sensitivity that allowed the detection of several classes of sources and to investigate new physics. This work reports the Citation: Bersanetti, D.; Patricelli, B.; main hardware upgrades of the detector and the main astrophysical results from the latest five years; Piccinni, O.J.; Piergiovanni, F.; future prospects for the Virgo detector are also presented.
    [Show full text]
  • Searching for the Neutron Star Or Black Hole Resulting from Gw170817
    SEARCHING FOR THE NEUTRON STAR OR BLACK HOLE RESULTING FROM GW170817 With the detection of a binary neutron star merger by the Advanced Laser Interferometer Gravitational Wave Observatory (LIGO) and Virgo, a natural question to ask is: what happened to the resulting object that was formed? The merger of two neutron stars can lead to four ultimate outcomes: (i) the prompt formation of a black hole, (ii) the formation of a "hypermassive" neutron star that collapses to a black hole in less than a second, (iii) the formation of a "supramassive" neutron star that collapses to a black hole on much longer timescales, (iv) the formation of a stable neutron star. Which of these four possibilities occurs depends on how much mass remains in the resulting object, as well as the composition and properties of matter inside neutron stars. Knowing the masses of the original two neutron stars before they merged, which can be measured from the gravitational wave signal detected, and under some assumptions about the compactness of neutron stars, it seems most likely that the resulting object was a hypermassive neutron star, although the other options cannot be excluded either. In this analysis, we search for gravitational waves from the post-merger object, and although we do not find anything, we set the groundwork for future searches when we have further improved the sensitivity of our detectors and where we might also observe a merger even closer to us. WHAT MIGHT WE EXPECT TO OBSERVE? Simulations tell us that the remnant object that results from merging binary neutron stars also emits gravitational waves.
    [Show full text]
  • And Ecclesiastical Cosmology
    GSJ: VOLUME 6, ISSUE 3, MARCH 2018 101 GSJ: Volume 6, Issue 3, March 2018, Online: ISSN 2320-9186 www.globalscientificjournal.com DEMOLITION HUBBLE'S LAW, BIG BANG THE BASIS OF "MODERN" AND ECCLESIASTICAL COSMOLOGY Author: Weitter Duckss (Slavko Sedic) Zadar Croatia Pусскй Croatian „If two objects are represented by ball bearings and space-time by the stretching of a rubber sheet, the Doppler effect is caused by the rolling of ball bearings over the rubber sheet in order to achieve a particular motion. A cosmological red shift occurs when ball bearings get stuck on the sheet, which is stretched.“ Wikipedia OK, let's check that on our local group of galaxies (the table from my article „Where did the blue spectral shift inside the universe come from?“) galaxies, local groups Redshift km/s Blueshift km/s Sextans B (4.44 ± 0.23 Mly) 300 ± 0 Sextans A 324 ± 2 NGC 3109 403 ± 1 Tucana Dwarf 130 ± ? Leo I 285 ± 2 NGC 6822 -57 ± 2 Andromeda Galaxy -301 ± 1 Leo II (about 690,000 ly) 79 ± 1 Phoenix Dwarf 60 ± 30 SagDIG -79 ± 1 Aquarius Dwarf -141 ± 2 Wolf–Lundmark–Melotte -122 ± 2 Pisces Dwarf -287 ± 0 Antlia Dwarf 362 ± 0 Leo A 0.000067 (z) Pegasus Dwarf Spheroidal -354 ± 3 IC 10 -348 ± 1 NGC 185 -202 ± 3 Canes Venatici I ~ 31 GSJ© 2018 www.globalscientificjournal.com GSJ: VOLUME 6, ISSUE 3, MARCH 2018 102 Andromeda III -351 ± 9 Andromeda II -188 ± 3 Triangulum Galaxy -179 ± 3 Messier 110 -241 ± 3 NGC 147 (2.53 ± 0.11 Mly) -193 ± 3 Small Magellanic Cloud 0.000527 Large Magellanic Cloud - - M32 -200 ± 6 NGC 205 -241 ± 3 IC 1613 -234 ± 1 Carina Dwarf 230 ± 60 Sextans Dwarf 224 ± 2 Ursa Minor Dwarf (200 ± 30 kly) -247 ± 1 Draco Dwarf -292 ± 21 Cassiopeia Dwarf -307 ± 2 Ursa Major II Dwarf - 116 Leo IV 130 Leo V ( 585 kly) 173 Leo T -60 Bootes II -120 Pegasus Dwarf -183 ± 0 Sculptor Dwarf 110 ± 1 Etc.
    [Show full text]
  • Arxiv:2009.06555V3 [Astro-Ph.CO] 1 Feb 2021
    KCL-PH-TH/2020-53, CERN-TH-2020-150 Cosmic String Interpretation of NANOGrav Pulsar Timing Data John Ellis,1, 2, 3, ∗ and Marek Lewicki1, 4, y 1Kings College London, Strand, London, WC2R 2LS, United Kingdom 2Theoretical Physics Department, CERN, Geneva, Switzerland 3National Institute of Chemical Physics & Biophysics, R¨avala10, 10143 Tallinn, Estonia 4Faculty of Physics, University of Warsaw ul. Pasteura 5, 02-093 Warsaw, Poland Pulsar timing data used to provide upper limits on a possible stochastic gravitational wave back- ground (SGWB). However, the NANOGrav Collaboration has recently reported strong evidence for a stochastic common-spectrum process, which we interpret as a SGWB in the framework of cosmic strings. The possible NANOGrav signal would correspond to a string tension Gµ 2 (4×10−11; 10−10) at the 68% confidence level, with a different frequency dependence from supermassive black hole mergers. The SGWB produced by cosmic strings with such values of Gµ would be beyond the reach of LIGO, but could be measured by other planned and proposed detectors such as SKA, LISA, TianQin, AION-1km, AEDGE, Einstein Telescope and Cosmic Explorer. Introduction: Stimulated by the direct discovery of for cosmic string models, discussing how experiments gravitational waves (GWs) by the LIGO and Virgo Col- could confirm or disprove such an interpretation. Upper laborations [1{8] of black holes and neutron stars at fre- limits on the SGWB are often quoted assuming a spec- 2=3 quencies f & 10 Hz, there is widespread interest in ex- trum described by a GW abundance proportional to f , periments exploring other parts of the GW spectrum.
    [Show full text]
  • Benjamin J. Owen - Curriculum Vitae
    BENJAMIN J. OWEN - CURRICULUM VITAE Contact information Mail: Texas Tech University Department of Physics & Astronomy Lubbock, TX 79409-1051, USA E-mail: [email protected] Phone: +1-806-834-0231 Fax: +1-806-742-1182 Education 1998 Ph.D. in Physics, California Institute of Technology Thesis title: Gravitational waves from compact objects Thesis advisor: Kip S. Thorne 1993 B.S. in Physics, magna cum laude, Sonoma State University (California) Minors: Astronomy, German Research advisors: Lynn R. Cominsky, Gordon G. Spear Academic positions Primary: 2015{ Professor of Physics & Astronomy Texas Tech University 2013{2015 Professor of Physics The Pennsylvania State University 2008{2013 Associate Professor of Physics The Pennsylvania State University 2002{2008 Assistant Professor of Physics The Pennsylvania State University 2000{2002 Research Associate University of Wisconsin-Milwaukee 1998{2000 Research Scholar Max Planck Institute for Gravitational Physics (Golm) Secondary: 2015{2018 Adjunct Professor The Pennsylvania State University 2012 (2 months) Visiting Scientist Max Planck Institute for Gravitational Physics (Hanover) 2010 (6 months) Visiting Associate LIGO Laboratory, California Institute of Technology 2009 (6 months) Visiting Scientist Max Planck Institute for Gravitational Physics (Hanover) Honors and awards 2017 Princess of Asturias Award for Technical and Scientific Research (with the LIGO Scientific Collaboration) 2017 Albert Einstein Medal (with the LIGO Scientific Collaboration) 2017 Bruno Rossi Prize for High Energy Astrophysics (with the LIGO Scientific Collaboration) 2017 Royal Astronomical Society Group Achievement Award (with the LIGO Scientific Collab- oration) 2016 Gruber Cosmology Prize (with the LIGO Scientific Collaboration) 2016 Special Breakthrough Prize in Fundamental Physics (with the LIGO Scientific Collabora- tion) 2013 Fellow of the American Physical Society 1998 Milton and Francis Clauser Prize for Ph.D.
    [Show full text]
  • 121012-AAS-221 Program-14-ALL, Page 253 @ Preflight
    221ST MEETING OF THE AMERICAN ASTRONOMICAL SOCIETY 6-10 January 2013 LONG BEACH, CALIFORNIA Scientific sessions will be held at the: Long Beach Convention Center 300 E. Ocean Blvd. COUNCIL.......................... 2 Long Beach, CA 90802 AAS Paper Sorters EXHIBITORS..................... 4 Aubra Anthony ATTENDEE Alan Boss SERVICES.......................... 9 Blaise Canzian Joanna Corby SCHEDULE.....................12 Rupert Croft Shantanu Desai SATURDAY.....................28 Rick Fienberg Bernhard Fleck SUNDAY..........................30 Erika Grundstrom Nimish P. Hathi MONDAY........................37 Ann Hornschemeier Suzanne H. Jacoby TUESDAY........................98 Bethany Johns Sebastien Lepine WEDNESDAY.............. 158 Katharina Lodders Kevin Marvel THURSDAY.................. 213 Karen Masters Bryan Miller AUTHOR INDEX ........ 245 Nancy Morrison Judit Ries Michael Rutkowski Allyn Smith Joe Tenn Session Numbering Key 100’s Monday 200’s Tuesday 300’s Wednesday 400’s Thursday Sessions are numbered in the Program Book by day and time. Changes after 27 November 2012 are included only in the online program materials. 1 AAS Officers & Councilors Officers Councilors President (2012-2014) (2009-2012) David J. Helfand Quest Univ. Canada Edward F. Guinan Villanova Univ. [email protected] [email protected] PAST President (2012-2013) Patricia Knezek NOAO/WIYN Observatory Debra Elmegreen Vassar College [email protected] [email protected] Robert Mathieu Univ. of Wisconsin Vice President (2009-2015) [email protected] Paula Szkody University of Washington [email protected] (2011-2014) Bruce Balick Univ. of Washington Vice-President (2010-2013) [email protected] Nicholas B. Suntzeff Texas A&M Univ. suntzeff@aas.org Eileen D. Friel Boston Univ. [email protected] Vice President (2011-2014) Edward B. Churchwell Univ. of Wisconsin Angela Speck Univ. of Missouri [email protected] [email protected] Treasurer (2011-2014) (2012-2015) Hervey (Peter) Stockman STScI Nancy S.
    [Show full text]