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Abstracts Connecting to the Boston University Network
20th Cambridge Workshop: Cool Stars, Stellar Systems, and the Sun July 29 - Aug 3, 2018 Boston / Cambridge, USA Abstracts Connecting to the Boston University Network 1. Select network ”BU Guest (unencrypted)” 2. Once connected, open a web browser and try to navigate to a website. You should be redirected to https://safeconnect.bu.edu:9443 for registration. If the page does not automatically redirect, go to bu.edu to be brought to the login page. 3. Enter the login information: Guest Username: CoolStars20 Password: CoolStars20 Click to accept the conditions then log in. ii Foreword Our story starts on January 31, 1980 when a small group of about 50 astronomers came to- gether, organized by Andrea Dupree, to discuss the results from the new high-energy satel- lites IUE and Einstein. Called “Cool Stars, Stellar Systems, and the Sun,” the meeting empha- sized the solar stellar connection and focused discussion on “several topics … in which the similarity is manifest: the structures of chromospheres and coronae, stellar activity, and the phenomena of mass loss,” according to the preface of the resulting, “Special Report of the Smithsonian Astrophysical Observatory.” We could easily have chosen the same topics for this meeting. Over the summer of 1980, the group met again in Bonas, France and then back in Cambridge in 1981. Nearly 40 years on, I am comfortable saying these workshops have evolved to be the premier conference series for cool star research. Cool Stars has been held largely biennially, alternating between North America and Europe. Over that time, the field of stellar astro- physics has been upended several times, first by results from Hubble, then ROSAT, then Keck and other large aperture ground-based adaptive optics telescopes. -
Arxiv:1011.1177V1
Astronomy & Astrophysics manuscript no. 15346 c ESO 2018 October 25, 2018 Modeling of the Vela complex including the Vela supernova remnant, the binary system γ2 Velorum, and the Gum nebula I. Sushch1,2, B. Hnatyk3, and A. Neronov4 1 Humboldt Universit¨at zu Berlin, Institut f¨ur Physik, Berlin, Germany 2 National Taras Shevchenko University of Kyiv, Department of Physics, Kyiv, Ukraine 3 National Taras Shevchenko University of Kyiv, Astronomical Observatory, Kyiv, Ukraine 4 ISDC, Versoix, Switzerland Received 07 July 2010; accepted 18 October 2010 ABSTRACT We study the geometry and dynamics of the Vela complex including the Vela supernova remnant (SNR), the binary system γ2 Velorum and the Gum nebula. We show that the Vela SNR belongs to a subclass of non-Sedov adiabatic remnants in a cloudy interstellar medium (ISM), the dynamics of which is determined by the heating and evaporation of ISM clouds. We explain observable charac- teristics of the Vela SNR with a SN explosion with energy 1.4 × 1050 ergs near the step-like boundary of the ISM with low intercloud densities (∼ 10−3 cm−3) and with a volume-averaged density of clouds evaporated by shock in the north-east (NE) part about four times higher than the one in the south-west (SW) part. The observed asymmetry between the NE and SW parts of the Vela SNR could be explained by the presence of a stellar wind bubble (SWB) blown by the nearest-to-the Earth Wolf-Rayet (WR) star in the γ2 Velorum system. We show that the size and kinematics of γ2 Velorum SWB agree with predictions of numerical calculations for 2 the evolution of the SWB of Mini = 35M⊙ star. -
A Simple Method of Determining Archaeoastronomical Alignments in the Field
A Simple Method of Determining Archaeoastronomical Alignments in the Field TIMOTHY P. SEYMOUR STEPHEN J. EDBERG As an aid in achieving this goal, we have EDITOR'S NOTE: While it is not nor developed the following simplified algebraic mally our policy to publish papers of a purely expressions, derived from spherical trigo methodological nature, the following paper is nometry, which can be used to determine useful to archaeologists with an interest in whether or not a celestial object (such as the archaeoastronotny and can be employed in sun, moon, or particular star) of possible sig making observations of the type described in nificance will rise or set at a point on the the preceding paper. horizon indicated by an apparent alignment. The only field equipment required consists of ECAUSE of the recent interest on the a surveyor's transit, a book of trigonometric B part of archaeologists in the possible tables or hand calculator with trigonometric astronomical significance of various archaeo functions, and an inexpensive star atlas. In logical features, field archaeologists are addition, a great deal of preliminary analysis beginning to look for possible archaeoastro can be accomplished prior to going into the nomical alignments with ever-increasing field with nothing more complex than a topo vigilance. This awareness has resulted in a graphic map and a protractor. number of notable discoveries in the past Two equations are used in the calculations; several years and promises many more as one is a simplified version of the other. Which research continues. However, archaeologists equation is more appropriate will depend upon in the field face a number of problems in their the topographic conditions prevailing at the efforts to identify and describe such sites, not site. -