DOCSLIB.ORG

News from the Society for Astronomical Sciences

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
News from the Society for Astronomical Sciences Society for Astronomical Sciences Newsletter January 2018 News from the Society for Astronomical Sciences Vol. 16 No.1 (January, 2018) Invitation to the Society for Astronomical Sciences 2018 Symposium and ALPO Annual Meeting The SAS Program Committee invites you to participate in the Society for Astronomical Sciences’ 37th Annual Symposium. The Symposium is the premier annual conference devoted to small-telescope astronomical re- search. This year will be a joint meet- ing with the Association of Lunar and Planetary Observers (ALPO). The Symposium brings together ama- teur astronomers who are engaged in scientific research, professional as- tronomers, educators and students for in-depth discussions of topics related to small-telescope research. It is an Technical Presentations: Friday and Call for Papers: 2018 SAS excellent venue for presenting recent Saturday (June 15-16) will be the results, discussing targets of observa- Technical Sessions, including paper Symposium and ALPO tional campaigns, describing instru- presentations and poster sessions. 2018 Conference mentation and data reduction/analysis Presentations and Posters will span methods, developing collaborations, the wide range of topics of interest to Papers are solicited on all aspects of and bringing together the community the small-telescope research commu- astronomical science that are (or can of practice to share expertise and ex- nity: solar-system objects, variable- be) pursued by observations with small perience. Almost any topic related to stars, and binary stars; instrumentation telescopes (less than 1-meter aper- astronomical research using modest for photometry, astrometry and spec- ture), such as telescopes is of interest to SAS. You troscopy; and related subjects. Investigations of variable stars, need not be an expert to benefit from eclipsing binary stars, double participating in the Symposium: one You can read the Proceedings from recent SAS Symposia, and view vide- stars and stellar systems goal of SAS is to provide a mentoring Investigations of exoplanets, as- environment, to enable you to make os of many recent Presentations, on the SAS website teroids and other solar system ob- valuable contributions to astronomical jects science. (www.SocAstroSci.org). Progress, status, and planning for Date & Location: The 2018 SAS Sponsors: SAS Sponsors – develop- upcoming events such as the Symposium will be held on Thursday- ers, suppliers, and retailers of astro- eclipse of VV Cephei and the Friday-Saturday, June 14-15-16, 2018 nomical equipment – will be on hand launch of TESS. at the Ontario Airport Hotel, Ontario with displays of their featured prod- Instrumentation for photometry, CA. ucts. astrometry, spectroscopy, polar- imetry, and fast-cadence observa- Workshops: Educational workshops Registration: Symposium Early Reg- istration will open February 15, 2018. tions (e.g. occultations) are being planned for Thursday (June Investigations of atmospheric ef- 14). Details will be on the SAS web- The registration link will be on the SAS website (www.SocAstroSci.org). fects, light-propagation and scat- site soon. tering, light pollution monitoring 1 Society for Astronomical Sciences Newsletter January 2018 Innovative use of astronomy in The following candidates will be pre- were registered for the Workshop, then undergraduate education. sented to the Membership for election the recording is free. If you were not a as Directors, to serve from June 2018 registered attendee, then the price is Format: Papers for Presentation con- through June, 2021: $25 per workshop. Contact Bob sist of a 20-minute presentation (in- Buchheim ([email protected]) for Robert Buchheim (President) cluding Q&A), and a written paper that the details. Robert Stephens (Treasurer) is published in the Symposium Pro- Robert Gill (Secretary) Keeping in Touch: The SAS Yahoo ceedings. Jerry Foote group (“SocAstroSci”) is a good way to Papers without Presentation are in- John Menke keep in touch with the members and cluded in the Proceedings, without oral Wayne Green participants. presentation. Dr. John C. Martin Kudos, Criticisms, or fresh Ideas? We Poster Papers will be on display Under SAS Bylaws, members may are looking forward to seeing you at throughout the Symposium, and can nominate additional candidates at the SAS-2018! be included in the Symposium Pro- meeting. If you intend to nominate a If you have any questions or ideas for ceedings book. candidate, please inform the Secretary (Robert Gill) before the June Symposi- the Symposium, ideas for Workshops Important Dates: um. If no alternate candidates are or Technical topics that you would like to see, or comments on any other sub- Abstract submission begins: January nominated, then those listed above may be approved by voice vote. jects related to the Symposium, please 15, 2018. share them with the Program Commit- Abstracts should be sent to: pro- tee at [email protected]. [email protected]. Indicate whether you propose a Paper with Reminders to the SAS Presentation, Paper without Presenta- Membership ... tion, or Poster. A Target for Your Observ- Membership Renewal: Even if you ing Schedule Abstracts due: March 15, 2018 can’t attend the annual Symposium, we value your support of the Society 113 Amalthea: This asteroid was Authors will be notified of acceptance for Astronomical Sciences, and your reported as a binary, based on a single by March 22. interest in small-telescope science. “miss” chord (plus 7 positive occulta- Final papers due: April 26, 2018 tion chords) observed during the occul- As an SAS member, you will receive a tation of March 14, 2017. Symposium Early Registration opens: bound copy of the Proceedings even if February 15, 2018 you cannot come to the Symposium. A confirmation of this observation would be valuable. The occultation You may propose more than one pa- Symposium Proceedings: Published predicted for 2018-04-14 (UT date) will per for presentation, but normally only proceedings from all recent Symposia be a tricky observation, with the target one Presentation per author will be are freely available in PDF format at quite low in the sky, but worth the ef- scheduled. There is no limit to the the PUBLICATIONS tab of the SAS web- fort. Details of the event are available number of Posters or Papers without site (www.SocAstroSci.org). from IOTA at Presentation. Symposium Videos: If you missed a http://www.asteroidoccultation.com/20 You can see the scope and content of recent Symposium, you can still watch 18_04/0414_113_54752.htm presentations from the 2016 Symposi- many of the presentation videos on the um by downloading the Proceedings SAS website at the PUBLICATIONS tab. from the SAS website Workshop Videos: Video recordings of (www.SocAstroSci.org) and viewing most of the Workshops from recent the videos of presentations (see be- years are available from SAS. If you low) Triennial Election of SAS Committee SAS is a non-profit public benefit cor- poration incorporated in California, which is managed by a Board of Direc- tors (numbering no more than 7 per- sons). The Directors are elected by the membership, for 3-year terms. The 2018 Symposium will include a brief business meeting to elect 7 Direc- tors to hold office for the next three years. 2 Society for Astronomical Sciences Newsletter January 2018 Remote Telescopes & Ed- BAA-AAVSO Joint Variable Preview: Narrow-Band Im- ucation Conference Star Meeting aging of H II Regions Here’s an opportunity that will probably The British Astronomical Association The search for highly supersonic be of interest to some of you. Summer meeting this year will feature shock-waves inside HII regions ap- a joint session with the American As- pears to be a potentially fruitful Pro-Am The 2nd annual Conference on Robot- sociation of Variable Star Observers. collaboration area. Such waves can ic Telescopes, Student Research and The meeting will be held July 7-8, be produced by stellar winds, jets and Education (RTSRE) will be held in 2018 (Saturday and Sunday) at the outflows powered by forming young Hilo, Hawai’i from July 23-25, 2018. University of Warwick in Coventry, stars (Herbig-Haro objects), known This conference series focuses on England. classes of stellar eruptions such as building a sustainable community FU-Orionis events, supernovae, or around the educational, technical, and The BAA Summer Meeting takes place new classes of explosions such as student research uses of robotic tele- on Saturday, the BAA/AAVSO Variable stellar dynamical interactions or mer- scopes. The conference will be co- Star Meeting on Saturday and Sunday. gers in compact stellar systems. located with the interNational Astron- While the two meetings run inde- omy Teaching Summit (iNATS) from pendently in adjacent lecture theatres, Ultra-deep narrow-band H-alpha, July 25-27, 2018 providing worldwide there are plenary sessions bringing [OIII], [SII], [OII] images of all HII re- networking opportunities and hands-on both groups together at the beginning gions would be useful, to search for workshops designed to expand educa- and end of Saturday. Note that it is shocks similar to those seen in Ou4. tors’ teaching strategy toolkit and possible to attend the Summer Meet- The goal is to reach surface brightness aimed at innovative astronomy profes- ing on Saturday and the second day of (sensitivity to emission) as faint or sors, teachers, and outreach profes- the Variable Star meeting on Sunday. fainter than 1E-17 erg s^-1. Doing so sionals. probably requires exposure of tens of You will find program and registration hours per field, per filter, but many Find more information at the RTSRE information at astro-imagers are doing that already. website: https://rtsre.net/ https://britastro.org/summer2018 Ultra-narrow-band filters with band- widths of order 10 to 30 Å (rather than the usual 80 to 100 Å) and slow f/ratios Northeast Astro-Imaging (higher than f/10 to avoid bandpass Conference shifts) would help to eliminate broad- band emission from stars and scat- This annual gathering will be held April tered light in the nebula.
Load more

Recommended publications
  • Mathématiques Et Espace
    Atelier disciplinaire AD 5 Mathématiques et Espace Anne-Cécile DHERS, Education Nationale (mathématiques) Peggy THILLET, Education Nationale (mathématiques) Yann BARSAMIAN, Education Nationale (mathématiques) Olivier BONNETON, Sciences - U (mathématiques) Cahier d'activités Activité 1 : L'HORIZON TERRESTRE ET SPATIAL Activité 2 : DENOMBREMENT D'ETOILES DANS LE CIEL ET L'UNIVERS Activité 3 : D'HIPPARCOS A BENFORD Activité 4 : OBSERVATION STATISTIQUE DES CRATERES LUNAIRES Activité 5 : DIAMETRE DES CRATERES D'IMPACT Activité 6 : LOI DE TITIUS-BODE Activité 7 : MODELISER UNE CONSTELLATION EN 3D Crédits photo : NASA / CNES L'HORIZON TERRESTRE ET SPATIAL (3 ème / 2 nde ) __________________________________________________ OBJECTIF : Détermination de la ligne d'horizon à une altitude donnée. COMPETENCES : ● Utilisation du théorème de Pythagore ● Utilisation de Google Earth pour évaluer des distances à vol d'oiseau ● Recherche personnelle de données REALISATION : Il s'agit ici de mettre en application le théorème de Pythagore mais avec une vision terrestre dans un premier temps suite à un questionnement de l'élève puis dans un second temps de réutiliser la même démarche dans le cadre spatial de la visibilité d'un satellite. Fiche élève ____________________________________________________________________________ 1. Victor Hugo a écrit dans Les Châtiments : "Les horizons aux horizons succèdent […] : on avance toujours, on n’arrive jamais ". Face à la mer, vous voyez l'horizon à perte de vue. Mais "est-ce loin, l'horizon ?". D'après toi, jusqu'à quelle distance peux-tu voir si le temps est clair ? Réponse 1 : " Sans instrument, je peux voir jusqu'à .................. km " Réponse 2 : " Avec une paire de jumelles, je peux voir jusqu'à ............... km " 2. Nous allons maintenant calculer à l'aide du théorème de Pythagore la ligne d'horizon pour une hauteur H donnée.
    [Show full text]
  • Arxiv:2012.09981V1 [Astro-Ph.SR] 17 Dec 2020 2 O
    Contrib. Astron. Obs. Skalnat´ePleso XX, 1 { 20, (2020) DOI: to be assigned later Flare stars in nearby Galactic open clusters based on TESS data Olga Maryeva1;2, Kamil Bicz3, Caiyun Xia4, Martina Baratella5, Patrik Cechvalaˇ 6 and Krisztian Vida7 1 Astronomical Institute of the Czech Academy of Sciences 251 65 Ondˇrejov,The Czech Republic(E-mail: [email protected]) 2 Lomonosov Moscow State University, Sternberg Astronomical Institute, Universitetsky pr. 13, 119234, Moscow, Russia 3 Astronomical Institute, University of Wroc law, Kopernika 11, 51-622 Wroc law, Poland 4 Department of Theoretical Physics and Astrophysics, Faculty of Science, Masaryk University, Kotl´aˇrsk´a2, 611 37 Brno, Czech Republic 5 Dipartimento di Fisica e Astronomia Galileo Galilei, Vicolo Osservatorio 3, 35122, Padova, Italy, (E-mail: [email protected]) 6 Department of Astronomy, Physics of the Earth and Meteorology, Faculty of Mathematics, Physics and Informatics, Comenius University in Bratislava, Mlynsk´adolina F-2, 842 48 Bratislava, Slovakia 7 Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, H-1121 Budapest, Konkoly Thege Mikl´os´ut15-17, Hungary Received: September ??, 2020; Accepted: ????????? ??, 2020 Abstract. The study is devoted to search for flare stars among confirmed members of Galactic open clusters using high-cadence photometry from TESS mission. We analyzed 957 high-cadence light curves of members from 136 open clusters. As a result, 56 flare stars were found, among them 8 hot B-A type ob- jects. Of all flares, 63 % were detected in sample of cool stars (Teff < 5000 K), and 29 % { in stars of spectral type G, while 23 % in K-type stars and ap- proximately 34% of all detected flares are in M-type stars.
    [Show full text]
  • A Basic Requirement for Studying the Heavens Is Determining Where In
    Abasic requirement for studying the heavens is determining where in the sky things are. To specify sky positions, astronomers have developed several coordinate systems. Each uses a coordinate grid projected on to the celestial sphere, in analogy to the geographic coordinate system used on the surface of the Earth. The coordinate systems differ only in their choice of the fundamental plane, which divides the sky into two equal hemispheres along a great circle (the fundamental plane of the geographic system is the Earth's equator) . Each coordinate system is named for its choice of fundamental plane. The equatorial coordinate system is probably the most widely used celestial coordinate system. It is also the one most closely related to the geographic coordinate system, because they use the same fun­ damental plane and the same poles. The projection of the Earth's equator onto the celestial sphere is called the celestial equator. Similarly, projecting the geographic poles on to the celest ial sphere defines the north and south celestial poles. However, there is an important difference between the equatorial and geographic coordinate systems: the geographic system is fixed to the Earth; it rotates as the Earth does . The equatorial system is fixed to the stars, so it appears to rotate across the sky with the stars, but of course it's really the Earth rotating under the fixed sky. The latitudinal (latitude-like) angle of the equatorial system is called declination (Dec for short) . It measures the angle of an object above or below the celestial equator. The longitud inal angle is called the right ascension (RA for short).
    [Show full text]
  • Astronomy 2008 Index
    Astronomy Magazine Article Title Index 10 rising stars of astronomy, 8:60–8:63 1.5 million galaxies revealed, 3:41–3:43 185 million years before the dinosaurs’ demise, did an asteroid nearly end life on Earth?, 4:34–4:39 A Aligned aurorae, 8:27 All about the Veil Nebula, 6:56–6:61 Amateur astronomy’s greatest generation, 8:68–8:71 Amateurs see fireballs from U.S. satellite kill, 7:24 Another Earth, 6:13 Another super-Earth discovered, 9:21 Antares gang, The, 7:18 Antimatter traced, 5:23 Are big-planet systems uncommon?, 10:23 Are super-sized Earths the new frontier?, 11:26–11:31 Are these space rocks from Mercury?, 11:32–11:37 Are we done yet?, 4:14 Are we looking for life in the right places?, 7:28–7:33 Ask the aliens, 3:12 Asteroid sleuths find the dino killer, 1:20 Astro-humiliation, 10:14 Astroimaging over ancient Greece, 12:64–12:69 Astronaut rescue rocket revs up, 11:22 Astronomers spy a giant particle accelerator in the sky, 5:21 Astronomers unearth a star’s death secrets, 10:18 Astronomers witness alien star flip-out, 6:27 Astronomy magazine’s first 35 years, 8:supplement Astronomy’s guide to Go-to telescopes, 10:supplement Auroral storm trigger confirmed, 11:18 B Backstage at Astronomy, 8:76–8:82 Basking in the Sun, 5:16 Biggest planet’s 5 deepest mysteries, The, 1:38–1:43 Binary pulsar test affirms relativity, 10:21 Binocular Telescope snaps first image, 6:21 Black hole sets a record, 2:20 Black holes wind up galaxy arms, 9:19 Brightest starburst galaxy discovered, 12:23 C Calling all space probes, 10:64–10:65 Calling on Cassiopeia, 11:76 Canada to launch new asteroid hunter, 11:19 Canada’s handy robot, 1:24 Cannibal next door, The, 3:38 Capture images of our local star, 4:66–4:67 Cassini confirms Titan lakes, 12:27 Cassini scopes Saturn’s two-toned moon, 1:25 Cassini “tastes” Enceladus’ plumes, 7:26 Cepheus’ fall delights, 10:85 Choose the dome that’s right for you, 5:70–5:71 Clearing the air about seeing vs.
    [Show full text]
  • The Detection of 13CO and Other Apparent Abundance Anomalies In
    The Detection of 13CO and Other Apparent Abundance Anomalies in the Secondary Stars of Long-Period Cataclysmic Variables Thomas E. Harrison1,2, Heather L. Osborne2 Department of Astronomy New Mexico State University, Box 30001, MSC 4500, Las Cruces, NM 88003-8001 Steve B. Howell WIYN Observatory and National Optical Astronomy Observatories, 950 North Cherry Avenue, Tucson, AZ 85726 Accepted for publication in the Astronomical Journal on 18 February, 2004 1Visiting Astronomer, Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc. (AURA) under cooperative agreement with the National Science Foundation. 2Visiting Astronomer at the Infrared Telescope Facility, which is operated by the University arXiv:astro-ph/0402470v1 19 Feb 2004 of Hawaii under contract from the National Aeronautics and Space Administration. Subject headings: cataclysmic variablesstars: infrared spectrastars: individual (V442 Centauri, SY Cancri, RU Pegasi, CH Ursae Majoris, MU Centauri, TT Crateris, AC Cancri, EM Cygni, V426 Ophiuchi, SS Cygni, BV Puppis, AH Herculis) Received ; accepted –2– ABSTRACT We present moderate resolution (R ≥ 1,800) infrared K-band spectra of twelve long-period (Porb ≥ 6 hr) cataclysmic variables. We detect absorption lines from the photospheres of the secondary stars in every system, even though two of them were undergoing outbursts. We have attempted to assign spectral types to each of the secondary stars, and these classifications are generally consistent with previous determinations/estimates. We find evidence for abundance anomalies that include enhancements and/or deficits for all of the species commonly found in K-band spectra of G- and K-type dwarfs.
    [Show full text]
  • The Brightest Stars Seite 1 Von 9
    The Brightest Stars Seite 1 von 9 The Brightest Stars This is a list of the 300 brightest stars made using data from the Hipparcos catalogue. The stellar distances are only fairly accurate for stars well within 1000 light years. 1 2 3 4 5 6 7 8 9 10 11 12 13 No. Star Names Equatorial Galactic Spectral Vis Abs Prllx Err Dist Coordinates Coordinates Type Mag Mag ly RA Dec l° b° 1. Alpha Canis Majoris Sirius 06 45 -16.7 227.2 -8.9 A1V -1.44 1.45 379.21 1.58 9 2. Alpha Carinae Canopus 06 24 -52.7 261.2 -25.3 F0Ib -0.62 -5.53 10.43 0.53 310 3. Alpha Centauri Rigil Kentaurus 14 40 -60.8 315.8 -0.7 G2V+K1V -0.27 4.08 742.12 1.40 4 4. Alpha Boötis Arcturus 14 16 +19.2 15.2 +69.0 K2III -0.05 -0.31 88.85 0.74 37 5. Alpha Lyrae Vega 18 37 +38.8 67.5 +19.2 A0V 0.03 0.58 128.93 0.55 25 6. Alpha Aurigae Capella 05 17 +46.0 162.6 +4.6 G5III+G0III 0.08 -0.48 77.29 0.89 42 7. Beta Orionis Rigel 05 15 -8.2 209.3 -25.1 B8Ia 0.18 -6.69 4.22 0.81 770 8. Alpha Canis Minoris Procyon 07 39 +5.2 213.7 +13.0 F5IV-V 0.40 2.68 285.93 0.88 11 9. Alpha Eridani Achernar 01 38 -57.2 290.7 -58.8 B3V 0.45 -2.77 22.68 0.57 144 10.
    [Show full text]
  • Be Stars Seen by Space Photometry
    Be Stars Seen by Space Photometry Thomas Rivinius1, Dietrich Baade2 and Alex C. Carciofi3 1. ESO | European Organisation for Astronomical Research in the Southern Hemisphere, Casilla 19001, Santiago 19, Chile 2. ESO | European Organisation for Astronomical Research in the Southern Hemisphere, Karl-Schwarzschild-Str. 2, 85748 Garching, Germany 3. Instituto de Astronomia, Geof´ısica e Ci^encias Atmosf´ericas, Universidade de S~ao Paulo, 05508-900, S~ao Paulo, SP, Brazil Classical Be stars are introduced as object class and their particular potential for space based photometry is highlighted. A brief summary of the various types of variability observed in Be stars makes clear that an interpretation of every single frequency as a pulsation mode falls short, instead there are as well purely circumstellar variations and those that originate in the immediate stellar to cir- cumstellar interaction region. In particular the latter offer great potential, as they are linked to one of the few remaining great riddles of Be stars, namely how they feed their disks. 1 Introduction The class of Be stars is simply defined as those non-supergiant B stars that at least once have shown Balmer line emission (see Rivinius et al., 2013, for a review). While this definition is very valuable for bulk classification of stars for which no high quality data is available, e.g., in the Magellanic Clouds, it is also very broad: Any circumstellar gas close to a B star and above some threshold density will produce line emission. In an attempt at a taxonomy that reflects our knowledge on how the gas was put and is kept close to the star (e.g., magnetically confined, an accretion disk, or a decretion disk), the class was subdivided.
    [Show full text]
  • Arxiv:0908.2624V1 [Astro-Ph.SR] 18 Aug 2009
    Astronomy & Astrophysics Review manuscript No. (will be inserted by the editor) Accurate masses and radii of normal stars: Modern results and applications G. Torres · J. Andersen · A. Gim´enez Received: date / Accepted: date Abstract This paper presents and discusses a critical compilation of accurate, fun- damental determinations of stellar masses and radii. We have identified 95 detached binary systems containing 190 stars (94 eclipsing systems, and α Centauri) that satisfy our criterion that the mass and radius of both stars be known to ±3% or better. All are non-interacting systems, so the stars should have evolved as if they were single. This sample more than doubles that of the earlier similar review by Andersen (1991), extends the mass range at both ends and, for the first time, includes an extragalactic binary. In every case, we have examined the original data and recomputed the stellar parameters with a consistent set of assumptions and physical constants. To these we add interstellar reddening, effective temperature, metal abundance, rotational velocity and apsidal motion determinations when available, and we compute a number of other physical parameters, notably luminosity and distance. These accurate physical parameters reveal the effects of stellar evolution with un- precedented clarity, and we discuss the use of the data in observational tests of stellar evolution models in some detail. Earlier findings of significant structural differences between moderately fast-rotating, mildly active stars and single stars, ascribed to the presence of strong magnetic and spot activity, are confirmed beyond doubt. We also show how the best data can be used to test prescriptions for the subtle interplay be- tween convection, diffusion, and other non-classical effects in stellar models.
    [Show full text]
  • Open Clusters
    Open Clusters Open clusters (also known as galactic clusters) are of tremendous importance to the science of astronomy, if not to astrophysics and cosmology generally. Star clusters serve as the "laboratories" of astronomy, with stars now all at nearly the same distance and all created at essentially the same time. Each cluster thus is a running experiment, where we can observe the effects of composition, age, and environment. We are hobbled by seeing only a snapshot in time of each cluster, but taken collectively we can understand their evolution, and that of their included stars. These clusters are also important tracers of the Milky Way and other parent galaxies. They help us to understand their current structure and derive theories of the creation and evolution of galaxies. Just as importantly, starting from just the Hyades and the Pleiades, and then going to more distance clusters, open clusters serve to define the distance scale of the Milky Way, and from there all other galaxies and the entire universe. However, there is far more to the study of star clusters than that. Anyone who has looked at a cluster through a telescope or binoculars has realized that these are objects of immense beauty and symmetry. Whether a cluster like the Pleiades seen with delicate beauty with the unaided eye or in a small telescope or binoculars, or a cluster like NGC 7789 whose thousands of stars are seen with overpowering wonder in a large telescope, open clusters can only bring awe and amazement to the viewer. These sights are available to all.
    [Show full text]
  • Arxiv:2006.10868V2 [Astro-Ph.SR] 9 Apr 2021 Spain and Institut D’Estudis Espacials De Catalunya (IEEC), C/Gran Capit`A2-4, E-08034 2 Serenelli, Weiss, Aerts Et Al
    Noname manuscript No. (will be inserted by the editor) Weighing stars from birth to death: mass determination methods across the HRD Aldo Serenelli · Achim Weiss · Conny Aerts · George C. Angelou · David Baroch · Nate Bastian · Paul G. Beck · Maria Bergemann · Joachim M. Bestenlehner · Ian Czekala · Nancy Elias-Rosa · Ana Escorza · Vincent Van Eylen · Diane K. Feuillet · Davide Gandolfi · Mark Gieles · L´eoGirardi · Yveline Lebreton · Nicolas Lodieu · Marie Martig · Marcelo M. Miller Bertolami · Joey S.G. Mombarg · Juan Carlos Morales · Andr´esMoya · Benard Nsamba · KreˇsimirPavlovski · May G. Pedersen · Ignasi Ribas · Fabian R.N. Schneider · Victor Silva Aguirre · Keivan G. Stassun · Eline Tolstoy · Pier-Emmanuel Tremblay · Konstanze Zwintz Received: date / Accepted: date A. Serenelli Institute of Space Sciences (ICE, CSIC), Carrer de Can Magrans S/N, Bellaterra, E- 08193, Spain and Institut d'Estudis Espacials de Catalunya (IEEC), Carrer Gran Capita 2, Barcelona, E-08034, Spain E-mail: [email protected] A. Weiss Max Planck Institute for Astrophysics, Karl Schwarzschild Str. 1, Garching bei M¨unchen, D-85741, Germany C. Aerts Institute of Astronomy, Department of Physics & Astronomy, KU Leuven, Celestijnenlaan 200 D, 3001 Leuven, Belgium and Department of Astrophysics, IMAPP, Radboud University Nijmegen, Heyendaalseweg 135, 6525 AJ Nijmegen, the Netherlands G.C. Angelou Max Planck Institute for Astrophysics, Karl Schwarzschild Str. 1, Garching bei M¨unchen, D-85741, Germany D. Baroch J. C. Morales I. Ribas Institute of· Space Sciences· (ICE, CSIC), Carrer de Can Magrans S/N, Bellaterra, E-08193, arXiv:2006.10868v2 [astro-ph.SR] 9 Apr 2021 Spain and Institut d'Estudis Espacials de Catalunya (IEEC), C/Gran Capit`a2-4, E-08034 2 Serenelli, Weiss, Aerts et al.
    [Show full text]
  • 00E the Construction of the Universe Symphony
    The basic construction of the Universe Symphony. There are 30 asterisms (Suites) in the Universe Symphony. I divided the asterisms into 15 groups. The asterisms in the same group, lay close to each other. Asterisms!! in Constellation!Stars!Objects nearby 01 The W!!!Cassiopeia!!Segin !!!!!!!Ruchbah !!!!!!!Marj !!!!!!!Schedar !!!!!!!Caph !!!!!!!!!Sailboat Cluster !!!!!!!!!Gamma Cassiopeia Nebula !!!!!!!!!NGC 129 !!!!!!!!!M 103 !!!!!!!!!NGC 637 !!!!!!!!!NGC 654 !!!!!!!!!NGC 659 !!!!!!!!!PacMan Nebula !!!!!!!!!Owl Cluster !!!!!!!!!NGC 663 Asterisms!! in Constellation!Stars!!Objects nearby 02 Northern Fly!!Aries!!!41 Arietis !!!!!!!39 Arietis!!! !!!!!!!35 Arietis !!!!!!!!!!NGC 1056 02 Whale’s Head!!Cetus!! ! Menkar !!!!!!!Lambda Ceti! !!!!!!!Mu Ceti !!!!!!!Xi2 Ceti !!!!!!!Kaffalijidhma !!!!!!!!!!IC 302 !!!!!!!!!!NGC 990 !!!!!!!!!!NGC 1024 !!!!!!!!!!NGC 1026 !!!!!!!!!!NGC 1070 !!!!!!!!!!NGC 1085 !!!!!!!!!!NGC 1107 !!!!!!!!!!NGC 1137 !!!!!!!!!!NGC 1143 !!!!!!!!!!NGC 1144 !!!!!!!!!!NGC 1153 Asterisms!! in Constellation Stars!!Objects nearby 03 Hyades!!!Taurus! Aldebaran !!!!!! Theta 2 Tauri !!!!!! Gamma Tauri !!!!!! Delta 1 Tauri !!!!!! Epsilon Tauri !!!!!!!!!Struve’s Lost Nebula !!!!!!!!!Hind’s Variable Nebula !!!!!!!!!IC 374 03 Kids!!!Auriga! Almaaz !!!!!! Hoedus II !!!!!! Hoedus I !!!!!!!!!The Kite Cluster !!!!!!!!!IC 397 03 Pleiades!! ! Taurus! Pleione (Seven Sisters)!! ! ! Atlas !!!!!! Alcyone !!!!!! Merope !!!!!! Electra !!!!!! Celaeno !!!!!! Taygeta !!!!!! Asterope !!!!!! Maia !!!!!!!!!Maia Nebula !!!!!!!!!Merope Nebula !!!!!!!!!Merope
    [Show full text]
  • Variability Survey of Brightest Stars in Selected OB Associations? Jaan Laur1, 2, Indrek Kolka1, Tõnis Eenmäe1, Taavi Tuvikene1, and Laurits Leedjärv1
    Astronomy & Astrophysics manuscript no. Laur2016_arxiv c ESO 2018 October 15, 2018 Variability survey of brightest stars in selected OB associations? Jaan Laur1; 2, Indrek Kolka1, Tõnis Eenmäe1, Taavi Tuvikene1, and Laurits Leedjärv1 1 Tartu Observatory, Observatooriumi 1, 61602 Tõravere, Estonia e-mail: [email protected] 2 Institute of Physics, University of Tartu, W. Ostwaldi Str 1, 50411 Tartu, Estonia ABSTRACT Context. The stellar evolution theory of massive stars remains uncalibrated with high-precision photometric observational data mainly due to a small number of luminous stars that are monitored from space. Automated all-sky surveys have revealed numerous variable stars but most of the luminous stars are often overexposed. Targeted campaigns can improve the time base of photometric data for those objects. Aims. The aim of this investigation is to study the variability of luminous stars at different timescales in young open clusters and OB associations. Methods. We monitored 22 open clusters and associations from 2011 to 2013 using a 0.25-m telescope. Variable stars were detected by comparing the overall light-curve scatter with measurement uncertainties. Variability was analysed by the light curve feature extraction tool FATS. Periods of pulsating stars were determined using the discrete Fourier transform code SigSpec. We then classified the variable stars based on their pulsation periods and available spectral information. Results. We obtained light curves for more than 20000 sources of which 354 were found to be variable. Amongst them we find 80 eclipsing binaries, 31 α Cyg, 13 β Cep, 62 Be, 16 slowly pulsating B, 7 Cepheid, 1 γ Doradus, 3 Wolf-Rayet and 63 late-type variable stars.
    [Show full text]