Feasibility of Transit Photometry of Nearby Debris Discs
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Collisional Modelling of the AU Microscopii Debris Disc
A&A 581, A97 (2015) Astronomy DOI: 10.1051/0004-6361/201525664 & c ESO 2015 Astrophysics Collisional modelling of the AU Microscopii debris disc Ch. Schüppler1, T. Löhne1, A. V. Krivov1, S. Ertel2, J. P. Marshall3;4, S. Wolf5, M. C. Wyatt6, J.-C. Augereau7;8, and S. A. Metchev9 1 Astrophysikalisches Institut und Universitätssternwarte, Friedrich-Schiller-Universität Jena, Schillergäßchen 2–3, 07745 Jena, Germany e-mail: [email protected] 2 European Southern Observatory, Alonso de Cordova 3107, Vitacura, Casilla 19001, Santiago, Chile 3 School of Physics, University of New South Wales, NSW 2052 Sydney, Australia 4 Australian Centre for Astrobiology, University of New South Wales, NSW 2052 Sydney, Australia 5 Institut für Theoretische Physik und Astrophysik, Christian-Albrechts-Universität zu Kiel, Leibnizstraße 15, 24098 Kiel, Germany 6 Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK 7 Université Grenoble Alpes, IPAG, 38000 Grenoble, France 8 CNRS, IPAG, 38000 Grenoble, France 9 University of Western Ontario, Department of Physics and Astronomy, 1151 Richmond Avenue, London, ON N6A 3K7, Canada Received 14 January 2015 / Accepted 12 June 2015 ABSTRACT AU Microscopii’s debris disc is one of the most famous and best-studied debris discs and one of only two resolved debris discs around M stars. We perform in-depth collisional modelling of the AU Mic disc including stellar radiative and corpuscular forces (stellar winds), aiming at a comprehensive understanding of the dust production and the dust and planetesimal dynamics in the system. Our models are compared to a suite of observational data for thermal and scattered light emission, ranging from the ALMA radial surface brightness profile at 1.3 mm to spatially resolved polarisation measurements in the visible. -
The Constellation Microscopium, the Microscope Microscopium Is A
The Constellation Microscopium, the Microscope Microscopium is a small constellation in the southern sky, defined in the 18th century by Nicolas Louis de Lacaille in 1751–52 . Its name is Latin for microscope; it was invented by Lacaille to commemorate the compound microscope, i.e. one that uses more than one lens. The first microscope was invented by the two brothers, Hans and Zacharius Jensen, Dutch spectacle makers of Holland in 1590, who were also involved in the invention of the telescope (see below). Lacaille first showed it on his map of 1756 under the name le Microscope but Latinized this to Microscopium on the second edition published in 1763. He described it as consisting of "a tube above a square box". It contains sixty-nine stars, varying in magnitude from 4.8 to 7, the lucida being Gamma Microscopii of apparent magnitude 4.68. Two star systems have been found to have planets, while another has a debris disk. The stars that now comprise Microscopium may formerly have belonged to the hind feet of Sagittarius. However, this is uncertain as, while its stars seem to be referred to by Al-Sufi as having been seen by Ptolemy, Al-Sufi does not specify their exact positions. Microscopium is bordered Capricornus to the north, Piscis Austrinus and Grus to the west, Sagittarius to the east, Indus to the south, and touching on Telescopium to the southeast. The recommended three-letter abbreviation for the constellation, as adopted Seen in the 1824 star chart set Urania's Mirror (lower left) by the International Astronomical Union in 1922, is 'Mic'. -
Research at the Belgrade Astronomical Observatory
ASTRONOMY AND SPACE SCIENCE eds. M.K. Tsvetkov, L.G. Filipov, M.S. Dimitrijevic,´ L.C.ˇ Popovic,´ Heron Press Ltd, Sofia 2007 Influence of Collisional Processes on the Astrophysical Plasma Spectra – Research at the Belgrade Astronomical Observatory M.S. Dimitrijevic´ Astronomical Observatory, Volgina 7, 11160 Belgrade, Serbia Abstract. Activities on the project “Influence of collisional processes on the astrophysical plasma spectra”, supported by the Ministry of Science and Envi- ronment protection from 1st January 2002 up to 31st December 2005 are re- viewed, including other scientific results of the project participants. 1 Research on the Influence of Collisional Processes on the Astro- physical Plasma Spectra on Belgrade Astronomical Observatory From 1. January 2002, activities on investigation of the influence of collisional processes on the astrophysical plasma spectra are organized at Belgrade astronomical observatory within the frame of the project with the same name, supported by the Ministry of Science and Environment protection of Serbia. Investigations made within the frame of the Project concern plasma in astrophysics, lab- oratory and technology and the corresponding modelling, determination and research of atomic and molecular processes, optical properties and spectra, with a particular accent on the role of collisional processes. The particular attention has been paid to the inves- tigation of spectral line profiles, broadened by collisions with charged particles (Stark effect). Such investigations are of interest for the diagnostics and modelling of stellar plasma, plasma in laboratory and technological plasma. Semiclasical perturbation and Modified semiempirical methods were used, tested and investigated. Stark broadening parameters, line width and shift, were determined for a large number of spectral lines of Ag I, Ar I, Cd I, Ga I, Ge I, Kr I, Ne I, F II, In II, Ne II, Ti II, Be III, Cd III, Co III, Cu III, F III, S III, Si III, Zn III, and Si IV. -
Flares on Active M-Type Stars Observed with XMM-Newton and Chandra
Flares on active M-type stars observed with XMM-Newton and Chandra Urmila Mitra Kraev Mullard Space Science Laboratory Department of Space and Climate Physics University College London A thesis submitted to the University of London for the degree of Doctor of Philosophy I, Urmila Mitra Kraev, confirm that the work presented in this thesis is my own. Where information has been derived from other sources, I confirm that this has been indicated in the thesis. Abstract M-type red dwarfs are among the most active stars. Their light curves display random variability of rapid increase and gradual decrease in emission. It is believed that these large energy events, or flares, are the manifestation of the permanently reforming magnetic field of the stellar atmosphere. Stellar coronal flares are observed in the radio, optical, ultraviolet and X-rays. With the new generation of X-ray telescopes, XMM-Newton and Chandra , it has become possible to study these flares in much greater detail than ever before. This thesis focuses on three core issues about flares: (i) how their X-ray emission is correlated with the ultraviolet, (ii) using an oscillation to determine the loop length and the magnetic field strength of a particular flare, and (iii) investigating the change of density sensitive lines during flares using high-resolution X-ray spectra. (i) It is known that flare emission in different wavebands often correlate in time. However, here is the first time where data is presented which shows a correlation between emission from two different wavebands (soft X-rays and ultraviolet) over various sized flares and from five stars, which supports that the flare process is governed by common physical parameters scaling over a large range. -
Curriculum Vitae John P
Curriculum Vitae John P. Blakeslee National Research Council of Canada Phone: 1-250-363-8103 Herzberg Astronomy & Astrophysics Programs Fax: 1-250-363-0045 5071 West Saanich Road Cell: 1-250-858-1357 Victoria, B.C. V9E 2E7 Email: [email protected] Canada Citizenship: USA Education 1997 Ph.D., Physics, Massachusetts Institute of Technology (supervisor: Prof. John Tonry) 1991 B. A., Physics, University of Chicago (Honors; supervisor: Prof. Donald York) Employment History 2007 – present Astronomer, Senior Research Officer NRC Herzberg Institute of Astrophysics 2008 – present Adjunct Associate Professor Department of Physics, University of Victoria 2008 – 2013 Adjunct Professor Washington State University 2005 – 2007 Assistant Professor of Physics Washington State University 2004 – 2005 Research Scientist Johns Hopkins University 2000 – 2004 Associate Research Scientist Johns Hopkins University 1999 – 2000 Postdoctoral Research Associate University of Durham, U.K. 1996 – 1999 Fairchild Postdoctoral Scholar California Institute of Technology Fellowships and Awards 2004 Ernest F. Fullam Award for Innovative Research in Astronomy, Dudley Observatory 2003 NASA Certificate for contributions to the success of HST Servicing Mission 3B 1996 – 1999 Sherman M. Fairchild Postdoctoral Fellowship in Astronomy, Caltech Professional Service 2016 – present Canadian Large Synoptic Survey Telescope (LSST) Consortium, Co-PI 2014 – present Chair, NOAO Time Allocation Committee (TAC) Extragalactic Panel 2008 – present National Representative, Gemini International -
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A&A 609, A8 (2018) Astronomy DOI: 10.1051/0004-6361/201731453 & c ESO 2017 Astrophysics The completeness-corrected rate of stellar encounters with the Sun from the first Gaia data release? C. A. L. Bailer-Jones Max Planck Institute for Astronomy, Königstuhl 17, 69117 Heidelberg, Germany e-mail: [email protected] Received 27 June 2017 / Accepted 12 August 2017 ABSTRACT I report on close encounters of stars to the Sun found in the first Gaia data release (GDR1). Combining Gaia astrometry with radial velocities of around 320 000 stars drawn from various catalogues, I integrate orbits in a Galactic potential to identify those stars which pass within a few parsecs. Such encounters could influence the solar system, for example through gravitational perturbations of the Oort cloud. 16 stars are found to come within 2 pc (although a few of these have dubious data). This is fewer than were found in a similar study based on Hipparcos data, even though the present study has many more candidates. This is partly because I reject stars with large radial velocity uncertainties (>10 km s−1), and partly because of missing stars in GDR1 (especially at the bright end). The closest encounter found is Gl 710, a K dwarf long-known to come close to the Sun in about 1.3 Myr. The Gaia astrometry predict a much closer passage than pre-Gaia estimates, however: just 16 000 AU (90% confidence interval: 10 000–21 000 AU), which will bring this star well within the Oort cloud. Using a simple model for the spatial, velocity, and luminosity distributions of stars, together with an approximation of the observational selection function, I model the incompleteness of this Gaia-based search as a function of the time and distance of closest approach. -
Observations and Modelling of a Large Optical Flare on at Microscopii
A&A 383, 548–557 (2002) Astronomy DOI: 10.1051/0004-6361:20011743 & c ESO 2002 Astrophysics Observations and modelling of a large optical flare on AT Microscopii D. Garc´ıa-Alvarez1, D. Jevremovi´c1,2,J.G.Doyle1, and C. J. Butler1 1 Armagh Observatory, College Hill, Armagh BT61 9DG N. Ireland e-mail: [email protected], [email protected], [email protected] 2 Astronomical Observatory, Volgina 7, 11070 Belgrade, Yugoslavia Received 26 September 2001 / Accepted 5 December 2001 Abstract. Spectroscopic observations covering the wavelength range 3600–4600 A˚ are presented for a large flare on the late type M dwarf AT Mic (dM4.5e). A procedure to estimate the physical parameters of the flaring plasma has been used which assumes a simplified slab model of the flare based on a comparison of observed and computed Balmer decrements. With this procedure we have determined the electron density, electron temperature, optical thickness and temperature of the underlying source for the impulsive and gradual phases of the flare. The magnitude and duration of the flare allows us to trace the physical parameters of the response of the lower atmosphere. In order to check our derived values we have compared them with other methods. In addition, we have also applied our procedure to a stellar and a solar flare for which parameters have been obtained using other techniques. Key words. stars: activity – stars: chromospheres – stars: flare – stars: late-type 1. Introduction (Doyle & Mathioudakis 1990; Byrne & McKay 1990). Even more energetic flares occur on the RS CVn binary Stellar flares are events where a large amount of energy is systems, the total flare energy in the largest of this type released in a short interval of time, radiating at almost of systems may exceed E ∼ 1038 erg (Doyle et al. -
1 the Effect of a Strong Stellar Flare on the Atmospheric Chemistry of An
The Effect of a Strong Stellar Flare on the Atmospheric Chemistry of an Earth-like Planet Orbiting an M dwarf (Astrobiology, accepted) Antígona Segura 1,* , Lucianne Walkowicz 2,* , Victoria Meadows 3,* , James Kasting 4,* , Suzanne Hawley 5 1Instituto de Ciencias Nucleares, Universidad Nacional Autónoma de México, 2University of California at Berkeley, 3University of Washington, 4Pennsylvania State University, 5University of Washington *Members of the Virtual Planet Laboratory Lead Team of the NASA Astrobiology Institute. To whom correspondence should be directed: Antígona Segura Universidad Nacional Autónoma de México Instituto de Ciencias Nucleares Circuito Exterior C.U. A.Postal 70-543 04510 México D.F. Phone: 52 (55) 5622 4739 ext. 269 Fax 52 (55) 56 22 46 82 E-mail: [email protected] Running title: Flare effect on an Earth-like planet Abstract Main sequence M stars pose an interesting problem for astrobiology: their abundance in our galaxy makes them likely targets in the hunt for habitable planets, but their strong chromospheric activity produces high energy radiation and charged particles that may be detrimental to life. We studied the impact of the 1985 April 12 flare from the M dwarf, AD Leonis (AD Leo), simulating the effects from both UV radiation and protons on the atmospheric chemistry of a hypothetical, Earth-like planet located within its habitable zone. Based on observations of solar proton events and the Neupert effect we estimated a proton flux associated with the flare of 5.9×10 8 protons cm -2 sr -1 s -1 for particles with energies >10MeV. Then we calculated the abundance of nitrogen oxides produced by the flare by scaling the production of these compounds during a large solar proton event called the “Carrington event”. -
Bibliography from ADS File: Doyle.Bib June 27, 2021 1
Bibliography from ADS file: doyle.bib Nelson, C. J., Doyle, J. G., & Erdélyi, R., “On the relationship between magnetic August 16, 2021 cancellation and UV burst formation”, 2016MNRAS.463.2190N ADS Hill, A., Byrnes, P., Fitzsimmons, J., et al., “A prototype of the NFIRAOS to instrument thermo-mechanical interface”, 2016SPIE.9912E..02H ADS Murphy, T., Kaplan, D. L., Stewart, A. J., et al., “The ASKAP Variables and Reid, A., Mathioudakis, M., Doyle, J. G., et al., “Magnetic Flux Cancellation in Slow Transients (VAST) Pilot Survey”, 2021arXiv210806039M ADS Ellerman Bombs”, 2016ApJ...823..110R ADS Vilangot Nhalil, N., Nelson, C. J., Mathioudakis, M., Doyle, J. G., & Ramsay, Shetye, J., Doyle, J. G., Scullion, E., et al., “High-cadence observations of G., “Power-law energy distributions of small-scale impulsive events on the spicular-type events on the Sun”, 2016A&A...589A...3S ADS active Sun: results from IRIS”, 2020MNRAS.499.1385V ADS Wedemeyer, S., Bastian, T., Brajša, R., et al., “Solar Science with the At- Ramsay, G., Doyle, J. G., & Doyle, L., “TESS observations of southern ultrafast acama Large Millimeter/Submillimeter Array-A New View of Our Sun”, rotating low-mass stars”, 2020MNRAS.497.2320R ADS 2016SSRv..200....1W ADS Doyle, L., Ramsay, G., & Doyle, J. G., “Superflares and variability in solar- Shetye, J., Doyle, J. G., Scullion, E., Nelson, C. J., & Kuridze, D., “High Ca- type stars with TESS in the Southern hemisphere”, 2020MNRAS.494.3596D dence Observations and Analysis of Spicular-type Events Using CRISP On- ADS board SST”, 2016ASPC..504..115S ADS Srivastava, A. K., Rao, Y. K., Konkol, P., et al., “Velocity Response of the Ob- Park, S. -
X-Raying the AU Microscopii Debris Disk
A&A 516, A8 (2010) Astronomy DOI: 10.1051/0004-6361/201014038 & c ESO 2010 Astrophysics X-raying the AU Microscopii debris disk P. C. Schneider and J. H. M. M. Schmitt Hamburger Sternwarte, Universität Hamburg, Gojenbergsweg 112, 21029 Hamburg, Germany e-mail: [email protected] Received 11 January 2010 / Accepted 24 March 2010 ABSTRACT AU Mic is a young, nearby X-ray active M-dwarf with an edge-on debris disk. Debris disk are the successors to the gaseous disks usually surrounding pre-main sequence stars which form after the first few Myrs of their host stars’ lifetime, when – presumably – also the planet formation takes place. Since X-ray transmission spectroscopy is sensitive to the chemical composition of the absorber, features in the stellar spectrum of AU Mic caused by its debris disk can in principle be detected. The upper limits we derive from our high resolution Chandra LETGS X-ray spectroscopy are on the same order as those from UV absorption measurements, consistent with the idea that AU Mic’s debris disk possesses an inner hole with only a very low density of sub-micron sized grains or gas. Key words. circumstellar matter – stars: individual: AU Microscopii – stars: coronae – X-rays: stars – protoplanetary disks 1. Introduction 1.2. AU Mic and its debris disk The first indications for cold material around AU Mic go The disks around young stars undergo dramatic changes during μ the first ∼10 Myr after their host stars’ birth, when the gas con- back to IRAS data, which exhibit excess emission at 60 m (Mathioudakis & Doyle 1991; Song et al. -
The Electric Sun Hypothesis
Basics of astrophysics revisited. II. Mass- luminosity- rotation relation for F, A, B, O and WR class stars Edgars Alksnis [email protected] Small volume statistics show, that luminosity of bright stars is proportional to their angular momentums of rotation when certain relation between stellar mass and stellar rotation speed is reached. Cause should be outside of standard stellar model. Concept allows strengthen hypotheses of 1) fast rotation of Wolf-Rayet stars and 2) low mass central black hole of the Milky Way. Keywords: mass-luminosity relation, stellar rotation, Wolf-Rayet stars, stellar angular momentum, Sagittarius A* mass, Sagittarius A* luminosity. In previous work (Alksnis, 2017) we have shown, that in slow rotating stars stellar luminosity is proportional to spin angular momentum of the star. This allows us to see, that there in fact are no stars outside of “main sequence” within stellar classes G, K and M. METHOD We have analyzed possible connection between stellar luminosity and stellar angular momentum in samples of most known F, A, B, O and WR class stars (tables 1-5). Stellar equatorial rotation speed (vsini) was used as main parameter of stellar rotation when possible. Several diverse data for one star were averaged. Zero stellar rotation speed was considered as an error and corresponding star has been not included in sample. RESULTS 2 F class star Relative Relative Luminosity, Relative M*R *eq mass, M radius, L rotation, L R eq HATP-6 1.29 1.46 3.55 2.950 2.28 α UMi B 1.39 1.38 3.90 38.573 26.18 Alpha Fornacis 1.33 -
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Volume 43 Number 1 JAAVSO 2015 The Journal of the American Association of Variable Star Observers The Curious Case of ASAS J174600-2321.3: an Eclipsing Symbiotic Nova in Outburst? Light curve of ASAS J174600-2321.3, based on EROS-2, ASAS-3, and APASS data. Also in this issue... • The Early-Spectral Type W UMa Contact Binary V444 And • The δ Scuti Pulsation Periods in KIC 5197256 • UXOR Hunting among Algol Variables • Early-Time Flux Measurements of SN 2014J Obtained with Small Robotic Telescopes: Extending the AAVSO Light Curve Complete table of contents inside... The American Association of Variable Star Observers 49 Bay State Road, Cambridge, MA 02138, USA The Journal of the American Association of Variable Star Observers Editor John R. Percy Edward F. Guinan Paula Szkody University of Toronto Villanova University University of Washington Toronto, Ontario, Canada Villanova, Pennsylvania Seattle, Washington Associate Editor John B. Hearnshaw Matthew R. Templeton Elizabeth O. Waagen University of Canterbury AAVSO Christchurch, New Zealand Production Editor Nikolaus Vogt Michael Saladyga Laszlo L. Kiss Universidad de Valparaiso Konkoly Observatory Valparaiso, Chile Budapest, Hungary Editorial Board Douglas L. Welch Geoffrey C. Clayton Katrien Kolenberg McMaster University Louisiana State University Universities of Antwerp Hamilton, Ontario, Canada Baton Rouge, Louisiana and of Leuven, Belgium and Harvard-Smithsonian Center David B. Williams Zhibin Dai for Astrophysics Whitestown, Indiana Yunnan Observatories Cambridge, Massachusetts Kunming City, Yunnan, China Thomas R. Williams Ulisse Munari Houston, Texas Kosmas Gazeas INAF/Astronomical Observatory University of Athens of Padua Lee Anne M. Willson Athens, Greece Asiago, Italy Iowa State University Ames, Iowa The Council of the American Association of Variable Star Observers 2014–2015 Director Arne A.