Thomas J. Maccarone Texas Tech
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
The AAVSO DSLR Observing Manual
The AAVSO DSLR Observing Manual AAVSO 49 Bay State Road Cambridge, MA 02138 email: [email protected] Version 1.2 Copyright 2014 AAVSO Foreword This manual is a basic introduction and guide to using a DSLR camera to make variable star observations. The target audience is first-time beginner to intermediate level DSLR observers, although many advanced observers may find the content contained herein useful. The AAVSO DSLR Observing Manual was inspired by the great interest in DSLR photometry witnessed during the AAVSO’s Citizen Sky program. Consumer-grade imaging devices are rapidly evolving, so we have elected to write this manual to be as general as possible and move the software and camera-specific topics to the AAVSO DSLR forums. If you find an area where this document could use improvement, please let us know. Please send any feedback or suggestions to [email protected]. Most of the content for these chapters was written during the third Citizen Sky workshop during March 22-24, 2013 at the AAVSO. The persons responsible for creation of most of the content in the chapters are: Chapter 1 (Introduction): Colin Littlefield, Paul Norris, Richard (Doc) Kinne, Matthew Templeton Chapter 2 (Equipment overview): Roger Pieri, Rebecca Jackson, Michael Brewster, Matthew Templeton Chapter 3 (Software overview): Mark Blackford, Heinz-Bernd Eggenstein, Martin Connors, Ian Doktor Chapters 4 & 5 (Image acquisition and processing): Robert Buchheim, Donald Collins, Tim Hager, Bob Manske, Matthew Templeton Chapter 6 (Transformation): Brian Kloppenborg, Arne Henden Chapter 7 (Observing program): Des Loughney, Mike Simonsen, Todd Brown Various figures: Paul Valleli Clear skies, and Good Observing! Arne Henden, Director Rebecca Turner, Operations Director Brian Kloppenborg, Editor Matthew Templeton, Science Director Elizabeth Waagen, Senior Technical Assistant American Association of Variable Star Observers Cambridge, Massachusetts June 2014 i Index 1. -
The Red Supergiant Content of the Local Group
The Lives and Death-throes of Massive Stars Proceedings IAU Symposium No. 329, 2017 c 2017 International Astronomical Union J.J.Eldridge,ed. DOI: 00.0000/X000000000000000X The Red Supergiant Content of the Local Group Philip Massey1, Emily Levesque2, Kathryn Neugent1, Kate Evans1,3, Maria Drout4, and Madeleine Beck5 1 Lowell Observatory, 1400 W Mars Hill Road, Flagstaff, AZ 86001 and Dept. Physics & Astronomy, Northern Arizona University, Flagstaff, AZ 86011-6010 email: [email protected], [email protected] 2Dept. Astronomy, University of Washington, Box 351580, Seattle, WA 98195 USA email: [email protected] 3REU participant, 2015; California Institute of Technology, 1200 E, California Blvd, Pasadena, CA 91125 USA email: [email protected] 4Observatories of the Carnegie Institution for Science, 813 Santa Barbara St., Pasadena, CA 91101, USA email:[email protected] 5REU participant, 2016; Wellesley College, 106 Central Street, Wellesley, MA 02481 USA email: [email protected] Abstract. We summarize here recent work in identifying and characterizing red supergiants (RSGs) in the galaxies of the Local Group. Keywords. stars: early type, supergiants, stars: Wolf-Rayet 1. Introduction In the Olden Days, the term “massive star” was synonymous with “hot [massive] star,” and topics at these conferences were restricted to O-type stars and Wolf-Rayet (WR) stars. Gradually massive star research has expanded to include the red supergiants (RSGs). Stars with initial masses 8 − 30M⊙ will evolve into RSGs, and these are the progenitors of many core-collapse SNe. The amount of mass loss during the RSG phase will affect the subsequent evolution (if any) of these stars, with some evolving back to the blue side of the H-R diagram (HRD), and possibly even becoming WRs (see, e.g., Meynet et al. -
A New Survey of Cool Supergiants in the Magellanic Clouds⋆
A&A 578, A3 (2015) Astronomy DOI: 10.1051/0004-6361/201425362 & c ESO 2015 Astrophysics A new survey of cool supergiants in the Magellanic Clouds? Carlos González-Fernández1, Ricardo Dorda2, Ignacio Negueruela2, and Amparo Marco2 1 Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK e-mail: [email protected] 2 Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Universidad de Alicante, Apdo. 99, 03080 Alicante, Spain Received 18 November 2014 / Accepted 31 March 2015 ABSTRACT Aims. In this study we conduct a pilot program aimed at the red supergiant population of the Magellanic Clouds. We intend to extend the current known sample to the unexplored low end of the brightness distribution of these stars, building a more representative dataset with which to extrapolate their behaviour to other Galactic and extra-galactic environments. Methods. We select candidates using only near infrared photometry, and with medium resolution multi-object spectroscopy, we perform spectral classification and derive their line-of-sight velocities, confirming the nature of the candidates and their membership in the clouds. Results. Around two hundred new red supergiants have been detected, hinting at a yet to be observed large population. Using near- and mid-infrared photometry we study the brightness distribution of these stars, the onset of mass-loss, and the effect of dust in their atmospheres. Based on this sample, new a priori classification criteria are investigated, combining mid- and near-infrared photometry to improve the observational efficiency of similar programs to this. Key words. supergiants – stars: massive – stars: late-type – stars: AGB and post-AGB – Magellanic Clouds – surveys 1. -
THE PROGENITORS of TYPE IIP SUPERNOVAE Emma R. Beasor
THE PROGENITORS OF TYPE IIP SUPERNOVAE Emma R. Beasor A thesis submitted in partial fulfilment of the requirements of Liverpool John Moores University for the degree of Doctor of Philosophy. April 2019 Declaration The work presented in this thesis was carried out at the Astrophysics Research Insti- tute, Liverpool John Moores University. Unless otherwise stated, it is the original work of the author. While registered as a candidate for the degree of Doctor of Philosophy, for which sub- mission is now made, the author has not been registered as a candidate for any other award. This thesis has not been submitted in whole, or in part, for any other degree. Emma R. Beasor Astrophysics Research Institute Liverpool John Moores University IC2, Liverpool Science Park 146 Brownlow Hill Liverpool L3 5RF UK ii Abstract Mass-loss prior to core collapse is arguably the most important factor affecting the evolution of a massive star across the Hertzsprung-Russel (HR) diagram, making it the key to understanding what mass-range of stars produce supernova (SN), and how these explosions will appear. It is thought that most of the mass-loss occurs during the red supergiant (RSG) phase, when strong winds dictate the onward evolutionary path of the star and potentially remove the entire H-rich envelope. Uncertainty in the driving mechanism for RSG winds means the mass-loss rate (M_ ) cannot be determined from first principles, and instead, stellar evolution models rely on empirical recipes to inform their calculations. At present, the most commonly used M_ -prescription comes from a literature study, whereby many measurements of mass- loss were compiled. -
2013 Version
Citizen Science with Variable Stars Brought to you by the AAVSO, Astronomers without Borders, the National Science Foundation and Your Universe Astronomers need your help! Many bright stars change in brightness all the time and for many different reasons. Some stars are too bright for professionals to CitizenSky is a collaboration of the look at with most large telescopes. So, we American Association of need your help to watch these stars as they Variable Star Observers (AAVSO), the University of dim and brighten over the next several years. Denver, the Adler Planetarium, the Johns Hopkins University and the California Academies of This guide will help you find these bright Science with support from the National Science Foundation. stars, measure their brightness and then submit the measurements to assist professional astronomers. Participate in one of the largest and longest running citizen science projects in history! Thousands of people just like you are helping o ut. Astronomers need large numbers of people to get the amount of precision they need to do their research. You are the key. Header artwork is reproduced with permission from Sky & Telescope magazine (www.skyandtelescope.com) Betelgeuse – Alpha Orionis From the city or country sky, from almost any part of the world, the majestic figure of Orion dominates the night sky with his belt, sword, and club. Low and to the right is the great red pulsating supergiant, Betelgeuse (alpha Orionis). Recently acquiring fame for being the first star to have its atmosphere directly imaged (shown below), alpha Orionis has captivated observers' attention for centuries. At minimum brightness, as in 1927 and 1941, its magnitude may drop below 1.2. -
NL#135 May/June
May/June 2007 Issue 135 A Publication for the members of the American Astronomical Society 3 IOP to Publish President’s Column AAS Journals J. Craig Wheeler, [email protected] Whew! A lot has happened! 5 Member Deaths First, my congratulations to John Huchra who was elected to be the next President of the Society. John will formally become President-Elect at the meeting in Hawaii. He will then take over as President at the meeting in St. Louis in June of 2008 and I will serve as Past-President until the 6 Pasadena meeting in June of 2009. We have hired a consultant to lead a one-day Council retreat before the Hawaii meeting to guide the Council toward a more strategic outlook for the Society. Seattle Meeting John has generously agreed to join that effort. I know he will put his energy, intellect, and experience Highlights behind the health and future of the Society. We had a short, intense, and very professional process to issue a Request for Proposals (RFP) to 10 publish the Astrophysical Journal and the Astronomical Journal, to evaluate the proposals, and Award Winners to select a vendor. We are very pleased that the IOP Publishing will be the new publisher of our cherished and prestigious journals and are very optimistic that our new partnership will lead to in Seattle a necessary and valuable evolution of what it means to publish science journals in the globally- connected electronic age. 11 The complex RFP defining our journals and our aspirations for them was put together by a team International consisting of AAS representatives and outside independent consultants. -
ATNF News Issue No
ATNF News Issue No. 66, April 2009 ISSN 1323-6326 See Compact Array Broadband Backend (CABB) article on page 6. Left to right: CABB Project Leader Dr Warwick Wilson, CSIRO Chief Executive Offi cer Megan Clark and ATNF Acting Director Dr Lewis Ball, with a CABB signal processing board in front of two antennas of the Australia Telescope Compact Array. Photo: Paul Mathews Photographics Removing the “spaghetti” of ribbon cable that fed the old correlator, from left to right, Matt Shields (obscured), Brett Hiscock, Scott Munting, Mark Leach, and Peter Mirtschin. Photo: CSIRO Cover page images CABB Project—team photo. Back row, left to right: Warwick Wilson (Project Leader), Paul Roberts, Grant Hampson, Peter Axtens, Yoon Chung. Middle row: Aaron Sanders, Dick Ferris (Project Engineer), Matt Shields, Mark Leach (Project Manager). Front row: Troy Elton, Andrew Brown, Raji Chekkala, Evan Davis. Other contributors (not in photo): Scott Saunders. (See article on page 6.) Photo: Tim Wheeler, April 2009 The Sunrise television crew prepare to broadcast live from the grounds of the CSIRO Parkes Observatory. Photo: Tim Ruckley, CSIRO Installation of a 300 – 900-MHz receiver on the Parkes 64-m radio telescope. (See article on page 28.) Photo: Maik Wolleben, CSIRO 2 ATNF News, Issue 66, April 2009 Contents Editorial.............................................................................................................................................................................3 From the Director ......................................................................................................................................................4 -
University Microfilms International 300 N
INFORMATION TO USERS This was produced from a copy of a document sent to us for microfilming. While the most advanced technological means to photograph and reproduce this document have been used, the quality is heavily dependent upon the quality of the material submitted. The following explanation of techniques is provided to help you understand markings or notations which may appear on this reproduction. 1. The sign or "target” for pages apparently lacking from the document photographed is “ Missing Page(s)”. If it was possible to obtain the missing page(s) or section, they are spliced into the film along with adjacent pages. This may have necessitated cutting through an image and duplicating adjacent pages to assure you of complete continuity. 2. When an image on the film is obliterated with a round black mark it is an indication that the film inspector noticed either blurred copy because of movement during exposure, or duplicate copy. Unless we meant to delete copyrighted materials that should not have been filmed, you will find a good image o f the page in the adjacent frame. If copyrighted materials were deleted you will find a target note listing the pages in the adjacent frame. 3. When a map, drawing or chart, etc., is part of the material being photo graphed the photographer has followed a definite method in “sectioning” the material. It is customary to begin filming at the upper left hand corner of a large sheet and to continue from left to right in equal sections with small overlaps. If necessary, sectioning is continued again—beginning below the first row and continuing on until complete. -
Newsletter 2021-2 April 2021
Newsletter 2021-2 April 2021 www.variablestarssouth.org A seemingly compelling sinusoidal fit to an O - C diagram for GZ Pup that may indicate a third body in the system. But all is not as it seems. Read on page 13 how Tom Richards, with the help of Jeff Byron, shows why this scenario just isn’t true. Contents From the Director - Mark Blackford .......................................................................................................................................................2 RASNZ Annual Conference – Steve Butler ...............................................................................................................................3 Identifications for five old variables – Mati Morel ..............................................................................................................4 The effects of master flats on the accuracy of DSLR photometry – Roy Axelsen ...........6 Refining the orbital period of KX Velorum – Mark Blackford ...........................................................................9 The cycle count error trap – Tom Richards ...........................................................................................................................14 Publication watch .........................................................................................................................................................................................................21 About ...............................................................................................................................................................................................................................................23 -
The Effective Temperature and the Absolute Magnitude of the Stars
Journal of High Energy Physics, Gravitation and Cosmology, 2016, 2, 66-74 Published Online January 2016 in SciRes. http://www.scirp.org/journal/jhepgc http://dx.doi.org/10.4236/jhepgc.2016.21007 The Effective Temperature and the Absolute Magnitude of the Stars Angel Fierros Palacios Instituto de Investigaciones Eléctricas, División de Energías Alternas, Mexico Received 4 June 2015; accepted 8 January 2016; published 12 January 2016 Copyright © 2016 by author and Scientific Research Publishing Inc. This work is licensed under the Creative Commons Attribution International License (CC BY). http://creativecommons.org/licenses/by/4.0/ Abstract The theoretical framework developed by A.S. Eddington for the study of the inner structure and stability of the stars has been modified by the author and used in this work to show that knowing the effective temperature and the absolute magnitude, the basic parameters of any gaseous star can be calculated. On the other hand, a possible theoretical explanation of the Hertzsprung-Russel Diagram is presented. Keywords The Effective Temperature and the Absolute Magnitude of the Stars 1. Introduction The study and understanding of the deep inner parts of the Sun and other stars is a physical situation which seems to be outside the reach of traditional scientific research methods. However, these celestial objects are con- tinuously sending out information to the outer space through the material barriers inside themselves, and this in- formation can be registered in the form of observational data. Therefore, it can be said that the interior of the stars is not disconnected from the rest of the Universe. -
A Strongly Heated Neutron Star in the Transient Z Source Maxi J0556-332
A STRONGLY HEATED NEUTRON STAR IN THE TRANSIENT Z SOURCE MAXI J0556-332 The MIT Faculty has made this article openly available. Please share how this access benefits you. Your story matters. Citation Homan, Jeroen, Joel K. Fridriksson, Rudy Wijnands, Edward M. Cackett, Nathalie Degenaar, Manuel Linares, Dacheng Lin, and Ronald A. Remillard. “A STRONGLY HEATED NEUTRON STAR IN THE TRANSIENT Z SOURCE MAXI J0556-332.” The Astrophysical Journal 795, no. 2 (October 22, 2014): 131. © 2014 The American Astronomical Society As Published http://dx.doi.org/10.1088/0004-637x/795/2/131 Publisher IOP Publishing Version Final published version Citable link http://hdl.handle.net/1721.1/94549 Terms of Use Article is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use. The Astrophysical Journal, 795:131 (12pp), 2014 November 10 doi:10.1088/0004-637X/795/2/131 C 2014. The American Astronomical Society. All rights reserved. Printed in the U.S.A. A STRONGLY HEATED NEUTRON STAR IN THE TRANSIENT Z SOURCE MAXI J0556–332 Jeroen Homan1, Joel K. Fridriksson2, Rudy Wijnands2, Edward M. Cackett3, Nathalie Degenaar4, Manuel Linares5,6, Dacheng Lin7, and Ronald A. Remillard1 1 MIT Kavli Institute for Astrophysics and Space Research, 77 Massachusetts Avenue 37-582D, Cambridge, MA 02139, USA; [email protected] 2 Anton Pannekoek Institute for Astronomy, University of Amsterdam, Postbus 94249, 1090 GE Amsterdam, The Netherlands 3 Department of Physics & Astronomy, Wayne -
The Black Hole Candidate IGR J17091-3624 Going to Quiescence
UvA-DARE (Digital Academic Repository) The black hole candidate IGR J17091-3624 going to quiescence Altamirano, D.; Wijnands, R.; Belloni, T. Publication date 2013 Document Version Final published version Published in The astronomer's telegram Link to publication Citation for published version (APA): Altamirano, D., Wijnands, R., & Belloni, T. (2013). The black hole candidate IGR J17091-3624 going to quiescence. The astronomer's telegram, 5112. http://www.astronomerstelegram.org/?read=5112 General rights It is not permitted to download or to forward/distribute the text or part of it without the consent of the author(s) and/or copyright holder(s), other than for strictly personal, individual use, unless the work is under an open content license (like Creative Commons). Disclaimer/Complaints regulations If you believe that digital publication of certain material infringes any of your rights or (privacy) interests, please let the Library know, stating your reasons. In case of a legitimate complaint, the Library will make the material inaccessible and/or remove it from the website. Please Ask the Library: https://uba.uva.nl/en/contact, or a letter to: Library of the University of Amsterdam, Secretariat, Singel 425, 1012 WP Amsterdam, The Netherlands. You will be contacted as soon as possible. UvA-DARE is a service provided by the library of the University of Amsterdam (https://dare.uva.nl) Download date:24 Sep 2021 ATel #5112: The black hole candidate IGR J17091-3624 going to quiescence This space for free for your Outside GCN conference.