DOCSLIB.ORG

General Disclaimer One Or More of the Following Statements May Affect

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text

Load more

General Disclaimer One or more of the Following Statements may affect this Document This document has been reproduced from the best copy furnished by the organizational source. It is being released in the interest of making available as much information as possible. This document may contain data, which exceeds the sheet parameters. It was furnished in this condition by the organizational source and is the best copy available. This document may contain tone-on-tone or color graphs, charts and/or pictures, which have been reproduced in black and white. This document is paginated as submitted by the original source. Portions of this document are not fully legible due to the historical nature of some of the material. However, it is the best reproduction available from the original submission. Produced by the NASA Center for Aerospace Information (CASI) i k f., _ ^ ^ _ ^y^ ^^ .^ ^ ^^ ^ ^. i ..,. ^^'^;^^^ Z rn ^ ^ ;(NASA — Ck-1+J$4$6J ^ONTFcIbUTFONS OF TfiE N76--G94$5 Q3SERVA3'QRX OF NE4i MEXICO 5 ?'iiTE JivIYETtSITY, THRU YOLC^Mr 1 , NQ. ^s, HnRII. 4 {Neu I;exico State N76 - 29695 L.^iv.) $4 ^ ^iC $5.00 CSCI. G3A ZJncias X3189 ^i6 U^i7 ^C3^tT'R^Q^1T^C?1^IS ^F ^^^ ^^^^^^^T^^^ ".aF h1E'Vof 1V^EXICC) STATE ^11^1iV'ERSlT`^ LAS CR^i^ES, I^EO/V NIEX^C;® ^^ao^ ^^. ' , '^ JUL 197 6 ^^ ^h RECE.IV ^ ^ ^; Volume 1 Apri 1 , 1976 `d ^^^ ^^t .^^+^' Number 4 Pub1 i shed by: The Astranamy Department ^8l ^ ^ b 4^'^ Box 4500, New Mexico Mate University Las Cruces, New Mexicfl 88003 This issue completes Volume 1. Future issues will bear the serial number onl,^, starting with the Number ^. ^ k ^ct`^^^c^^T' ^ w ^-, Z rn G ,^ tij a ^ERS o CONTRIBUTIONS OF THE 0 B ^ E RVATO RY OF NEW MEXICO STATE UNIVERSITY lAS CRUCES, NEW MEXICO 88003 Volume 1 April, 19'6 Number 4 Published oy: The Astronomy Department Box 4500, New Mexico State University Las Cruces, New Mexico 88003 This issue completes Volume 1. Future issues will bear the serial number only, st^.rting with the Number 5. i ^ ^ ^ t CONTRIBUTTONS OF THE OBSERVATORY, NE^dI^^XTCO STATE UNIVERSTTY Volume 1, dumber ^ April 1976 TABLE OF CONTENTS Page Non-LTE Proi=ilex of Strong Solar Lines. 110 T. J. ScTzneeberger and H. .^. Beebe Emissivi'^ies and Detectability of the Pure Rotational Transitions oi• Molecular Hydrogen. 123 T. J, Schneeber^ger Photometry oi= R Coronae Borealis. 134 D. W. Datvsor, and E. ^'. Tedesco Intermediate-Band Photometry of Faint Standard Stars. 14.0 D. W. Da^vson Seyt'ert Galaxies --- A Study of Brightness Variation and Stel i ar Concentration . 143 D. W. Darvsora Testing ofi a Photoelectric Photometer I. Determination of Operational Parameters. 148 D. W, Dc^son rand E. F. Tedesco II. Observational Testing. la4 D. W. rDaaJSOn and E. '.^'. Tedesco Photometric Calibration_o-^ Planetary Photographs. 1a9 R. F'. Beebe i - Impravemertt o-F the Rhodes l6-inch Telescope on Tortu^a5 Mountain 7 64©mi T . C. W. Tombaugh The ^[ASA-NMSU Automated Meteor ^bseYwatory. : i66 - G, A. Harvey. - NASA.Langley Research Center J. Gaffey Now Mexico Sate llniversity - Measurements of ^3upiter `s Long:-Lived Features and C^Irrents, T76 _ E. ' J. Reese and R: F. Beebe. '^ i Published by: As^ronamy Department Box 4500, - New Mexico State University Las Cruces, New Mexi co"g$003 - - _. .. - .. , ^: .. ^ .. This -issue comple^es ` Vol ume l: Future issues will bear I±he serial number anZy, starting 4vi th liur^ber 5. - ;=! } ^.._^^ :, i a T. J. 5chne^berger and Id. A. Beebe a -; Depari:ment of Astronomy New Mex^ca State Un^vers^ty, has Cruces, N.^f. 880x3 I I I ! i } ^ is ^ ^ III. The Model A-^mosphere ^ .. .. .__. ^ .. ,- 3 ^ r 5. Altrock and Canfield ^ 1 974) / • (1969 ' • Athay and ^anfiald .. ' ' Li p sky and Avrett (1970) .. .. Lites (1973) ^ • • • - -adopt®d . ^ • ^ 3. ^ ' ^ .• .^ • .- ^kr^/sec) .,^ e •^ • ' . , s . ^ ' • • .^ • • .. • • • • • • e s 4 • • • ^ • 0. ^ 0. 500. 1000. 1500. H^km^ Fig. 1. Microturbulence models, velocity (km/sec) vs. height (km). Neight is defined as in the HSRA. The adapted model follows Lites' in the photosphere and low chromosphere, and is the joined via the dashed line to the Li p sky-Avrett model. 114 t i { ^ i' ^ t ^ ^_ ^ ^ ^ ` - _ _ ^ ^ t 'i r ^ i - \ 1 _l ci Ca ^I 'three bevels pl us a continuum were included in the Ca r^ model, The bound levels are 4s ZS^fz' 3d 2 D5 f2 and 4p 2 P3/z . Detailed calculations ° ° were made i=ar the [^ 7 i ne, 393.0 A, the infrared tripl et ^ i ne at $452.7 A, and the 4s 25If2 -^ continuum transition. R v -^ dapendence was assumed for the rantinuum transition, and the pha^aianizatipn crass sect=on at the. coati nuuni- head +gas taken to be 7.1 x l 0^' 1 ' cm2 . The remaining ^ ^ ee-bound continaa were co^npute^ with fired rates; with TRRD = 5G00°K. The phatow ionization cross sections and coli%sionaT - crass sections were adopted from Auer, Heasley, and Mlkey (1.972). The Van der Waals dispersion constant for bath line transitions-was set at l.3 x 10 -32 ^Weideman, 1955}. ____e } ^^__^ z The h and k l i nes of Mg I i were cal cul aced i ^ detai 1 uti'^ i zi ng the model atom ar^d atomic data of Mi lkey and hlihalas X1974). This model includes the 3s zS^1Z' 3p Zp ^fz , 3p and can^it^uUm levels. Fixed zP°9f2 ti I I ^^ ^(a I X5890., Ca I ^9-227., Mg I A5172., Ca II X3933., and Ca II x8542., _ respectivEly, at disk center. The cores of i;he D 2 , 1t422T, and b 2 transitions are forr^^ed i n the 1 borer chrbmasphere. The line center optical depths, T o , become usual to unity for these transitions at te^iperatures and heights abode the temperature minimum. We have ' 0 (5890} = 1 at THSRA = 5200°K, ^e o (4227} = 1 at TNSRA 5000°K and zQ (5172) ^ 1 at TBSRA = 4700°K. The computed cores of these lines are darker than observed. It is well known that the microturbulent velocity gradient can effect the core brightness of lines and preliminary calculations with Ca i indicate that a microturbulence model with a steep gradient similar to that used by Altrock and Canfield {1.974) (see Figure 1) wi 17 produce the observed .core i n-^ensi ty of 1:4227.. at ^ ► l _0. The computes! Doppler cores _are wide compared to observations for both Ca I and.. Mg I. The wings of DZ , X4227., and b 2 are in reasonable agreement with observation Tests with Mg i X5172 have shown that the agreement can be 3 . e_ _ _ . ___.^.____e_ _r _ __._^^_ ^_.__.Y _^._._ 1L_ tl_._ .1 _._ 1.1 ..... 'l ... 1 .8 .a ^^ ,4 .2 0 .1 .2 .3 .^4 .5 ^ ,2 ,4 .6 ,8 1.0 n A a a► '.^ - ^ Fig. 2. pbserved (dashed) and computed {solid) profiles of tla [ 45090., Fig. 3, p6served (dashed} and computed {solid} profilos of Ca 1 x4227., ;:^ where I^ is Lhe ratio of tine to continuum intensity, at disk center. where I, is the ratio of lfrse to continuun intensity, at disk center. 3 i ,a I ^ l ^ i ,35 .d ii ^^ ,4 ^^ .10 .2 ,43 - 1 ^' r ,2 ,d .6 ,8 - 1.0 '.i 1 ^A .1 ,2 ,3 .,^ Fig. 4. Observed (dashed} and cnr^uted (solid) profiles of Mg [ 7,51'2., ^^ where I * 1s the ratio of lino to centinwrn intensity, at disk center. Fig. 5, p hsorved {dashed} and computed (solid} profiles of Ca II x3933., where T„ is the ratio of ilne to tontinumo intensity, at disk center. _. 119 .^ ! . _...... __. ^ 3 ^^ Figure 6 displays the results for the 78542 transition of Ca II. This line is not expected to show strong coherency effects. The Doppler care is in good agreement with observation, but the wing is tnn bright. This may be due to the collisinnal broadening parameters we have used. 9 We compare in Figure 7 our calculated Mg II J^2795 profile to the :1 computed profile obtained by Milkey and Mihalas (1974) in the complete ^ y redistribution case. Comparision with observations is, as with Ca Ii K, poor but the comparison does provide a consistency check. The differences ^ between the two calculations are smal7 k and are due mainly to the choice ^ l of a mic^,oturbulence model. Again, as with Ca II, partial redistribution ^ effects rrEay be Important for the Mg II h and k lines. ^^ The -transitions we have calculated in detail represent a wide range in core formation heights and wavelength. The results of this study provide a background for calculations which account explicitly for the ^ i inhomogerenusstructure of the chromosphere. The resulting two component chromosphere will then be restrained by this grid of line profiles. ', VI. Acknowledgments The authors wish to thank Dr, R. W, Milkey for helpful discussions. The assistance of the H.M.S.U. Computer Center staff is gratefully acknowledged. This work was supported by NSF Grant Ian. Lp-43815. `^ l 20 ^' ^ i r ^ r ^ ^ ^ ., f r ^ ~ r • ^* ,d ^f • ,^ ,^ ,C1 ^^ ] ® /► . - Fig. G. U6served (dashed} and computed (solid} profiles of Ca II a854Z., t^ihere I^ is the ratio of line to continuum intensity, at disk center. O i e 1 ^ ^ .1 .2 .3 ,4 ,5 ^^ Fig. 7. the results of Milkey and Mihaias (1974) with complete redistribution (dashed) and the profile computed in this study (solid) far Mg II aZ852., where I is intensity x l0' in ergs/cm^/sec/star /Hz at dis^C center.
Recommended publications
  • 145, September 2010

    145, September 2010

    British Astronomical Association VARIABLE STAR SECTION CIRCULAR No 145, September 2010 Contents EG Andromedae Light Curve ................................................... inside front cover From the Director ............................................................................................... 1 Letter Page. Visual Observing ............................................................................ 4 Epsilon Aurigae Spectroscopically at Mid Eclipse .......................................... 5 Eclipsing Binary News ...................................................................................... 7 AO Cassiopeiae Phase Diagram ............................................................ 9 PV Cephei and Gyulbudaghian’s Nebula ........................................................ 10 WR140 Periastron Campaign Update .............................................................. 12 VSS Meeting, Pendrell Hall. The Central Stars of Planetary Nebulae ............ 14 RR Coronae Borealis 1993-2004 ...................................................................... 16 TU Cassiopeiae Phase Diagram 2005-2010 ..................................................... 18 Binocular Priority List ..................................................................................... 19 Eclipsing Binary Predictions ............................................................................ 20 Charges for Section Publications .............................................. inside back cover Guidelines for Contributing to the Circular .............................
  • FY08 Technical Papers by GSMTPO Staff

    FY08 Technical Papers by GSMTPO Staff

    AURA/NOAO ANNUAL REPORT FY 2008 Submitted to the National Science Foundation July 23, 2008 Revised as Complete and Submitted December 23, 2008 NGC 660, ~13 Mpc from the Earth, is a peculiar, polar ring galaxy that resulted from two galaxies colliding. It consists of a nearly edge-on disk and a strongly warped outer disk. Image Credit: T.A. Rector/University of Alaska, Anchorage NATIONAL OPTICAL ASTRONOMY OBSERVATORY NOAO ANNUAL REPORT FY 2008 Submitted to the National Science Foundation December 23, 2008 TABLE OF CONTENTS EXECUTIVE SUMMARY ............................................................................................................................. 1 1 SCIENTIFIC ACTIVITIES AND FINDINGS ..................................................................................... 2 1.1 Cerro Tololo Inter-American Observatory...................................................................................... 2 The Once and Future Supernova η Carinae...................................................................................................... 2 A Stellar Merger and a Missing White Dwarf.................................................................................................. 3 Imaging the COSMOS...................................................................................................................................... 3 The Hubble Constant from a Gravitational Lens.............................................................................................. 4 A New Dwarf Nova in the Period Gap............................................................................................................
  • The X-Ray Universe 2017

    The X-Ray Universe 2017

    The X-ray Universe 2017 6−9 June 2017 Centro Congressi Frentani Rome, Italy A conference organised by the European Space Agency XMM-Newton Science Operations Centre National Institute for Astrophysics, Italian Space Agency University Roma Tre, La Sapienza University ABSTRACT BOOK Oral Communications and Posters Edited by Simone Migliari, Jan-Uwe Ness Organising Committees Scientific Organising Committee M. Arnaud Commissariat ´al’´energie atomique Saclay, Gif sur Yvette, France D. Barret (chair) Institut de Recherche en Astrophysique et Plan´etologie, France G. Branduardi-Raymont Mullard Space Science Laboratory, Dorking, Surrey, United Kingdom L. Brenneman Smithsonian Astrophysical Observatory, Cambridge, USA M. Brusa Universit`adi Bologna, Italy M. Cappi Istituto Nazionale di Astrofisica, Bologna, Italy E. Churazov Max-Planck-Institut f¨urAstrophysik, Garching, Germany A. Decourchelle Commissariat ´al’´energie atomique Saclay, Gif sur Yvette, France N. Degenaar University of Amsterdam, the Netherlands A. Fabian University of Cambridge, United Kingdom F. Fiore Osservatorio Astronomico di Roma, Monteporzio Catone, Italy F. Harrison California Institute of Technology, Pasadena, USA M. Hernanz Institute of Space Sciences (CSIC-IEEC), Barcelona, Spain A. Hornschemeier Goddard Space Flight Center, Greenbelt, USA V. Karas Academy of Sciences, Prague, Czech Republic C. Kouveliotou George Washington University, Washington DC, USA G. Matt Universit`adegli Studi Roma Tre, Roma, Italy Y. Naz´e Universit´ede Li`ege, Belgium T. Ohashi Tokyo Metropolitan University, Japan I. Papadakis University of Crete, Heraklion, Greece J. Hjorth University of Copenhagen, Denmark K. Poppenhaeger Queen’s University Belfast, United Kingdom N. Rea Instituto de Ciencias del Espacio (CSIC-IEEC), Spain T. Reiprich Bonn University, Germany M. Salvato Max-Planck-Institut f¨urextraterrestrische Physik, Garching, Germany N.
  • Catching Stellar Mergers at Work with the Very Large Telescope

    Catching Stellar Mergers at Work with the Very Large Telescope

    Astronomical Science Catching Stellar Mergers at Work with the Very Large Telescope Interferometer Florentin Millour1 ing the inner hundreds of astronomical The 2002 eruption has been interpreted 1 Eric Lagadec units, exactly where discs and com- as the merger of a star of ~ 8 MA with a Orsola de Marco2 panions occur and are intimately related subsolar mass star (Tylenda & Soker, Dipankar P. K. Banerjee3 to the evolution of the stars. Interferome- 2006). Djamel Mékarnia1 try is ideally suited to resolve discs in the Alain Spang1 core of nebulae around stars of a range V838 Mon is embedded in a dense, large- Olivier Chesneau1† of masses from low to high. Here we pre- scale environment that was lit up by the sent a snapshot of two such objects — light echoes resulting from the 2002 erup- the R Coronae Borealis (RCB) star V838 tion (Bond et al., 2003), and potentially 1 Laboratoire Lagrange, UMR 7293, Univ. Cen and the eruptive variable V838 Mon contaminates observations of the central Nice Sophia-Antipolis, CNRS, Observa- — highlighting the seminal contribution star. High angular resolution studies with a toire de la Côte d’Azur, Nice, France of the astronomer Olivier Chesneau, who small field of view of a few arcseconds are 2 Department of Physics & Astronomy, passed away earlier this year. an asset in isolating the central regions Macquarie University, Sydney, Australia from the extended dusty cloud. A great 3 Astronomy & Astrophysics Division, The R Coronae Borealis stars are hydro- advantage of optical interferometry studies Physical Research Laboratory, gen-deficient carbon-rich supergiants, is thus to isolate the measurements from Navrangpura, India best known for their spectacular declines the extended environment.
  • Photometry of R Coronae Borealis Stars During the Recovery Phase of Their Declines

    Photometry of R Coronae Borealis Stars During the Recovery Phase of Their Declines

    CSIRO PUBLISHING www.publish.csiro.au/journals/pasa Publications of the Astronomical Society of Australia, 2003, 20, 159–164 Photometry of R Coronae Borealis Stars during the Recovery Phase of their Declines Lj. Skuljan, P. L. Cottrell, A. C. Gilmore and P. M. Kilmartin Department of Physics and Astronomy, University of Canterbury, Christchurch, New Zealand [email protected] [email protected] [email protected] [email protected] Received 2002 July 22, accepted 2003 January 14 Abstract: The photometric observations (UBVRI) of nine cool R Coronae Borealis (RCB) stars have been collected at Mt John University Observatory, New Zealand, over a period of twelve years. The analysis of the magnitude–colour and colour–colour diagrams for the recovery phase demonstrates that all declines exhibit a similar asymptotic approach to their normal brightness. Declines return to maximum brightness along a line with essentially the same slope that does not depend on the star or the depth of the decline. Assuming a uniform obscuration of the photosphere by the dust cloud during the recovery phase, the extinction properties of the material were determined. The ratio of total to selective extinction (RV) for the RCB stars in our sample is in the range 2.5 to 4.6, indicating that the obscuring dust has extinction properties similar to that of the interstellar dust. Observations have been compared with the theoretical extinction curves for different sorts of grains. Keywords: stars: variables: R Coronae Borealis — methods: data analysis 1 Introduction 2 Observations The R Coronae Borealis (RCB) stars are hydrogen- The photometric observations (UBV and UBVRI) of the deficient carbon-rich supergiants, with a characteristic nine RCB stars (Table 1) have been obtained at Mt John pattern of variability.
  • September 2020 BRAS Newsletter

    September 2020 BRAS Newsletter

    A Neowise Comet 2020, photo by Ralf Rohner of Skypointer Photography Monthly Meeting September 14th at 7:00 PM, via Jitsi (Monthly meetings are on 2nd Mondays at Highland Road Park Observatory, temporarily during quarantine at meet.jit.si/BRASMeets). GUEST SPEAKER: NASA Michoud Assembly Facility Director, Robert Champion What's In This Issue? President’s Message Secretary's Summary Business Meeting Minutes Outreach Report Asteroid and Comet News Light Pollution Committee Report Globe at Night Member’s Corner –My Quest For A Dark Place, by Chris Carlton Astro-Photos by BRAS Members Messages from the HRPO REMOTE DISCUSSION Solar Viewing Plus Night Mercurian Elongation Spooky Sensation Great Martian Opposition Observing Notes: Aquila – The Eagle Like this newsletter? See PAST ISSUES online back to 2009 Visit us on Facebook – Baton Rouge Astronomical Society Baton Rouge Astronomical Society Newsletter, Night Visions Page 2 of 27 September 2020 President’s Message Welcome to September. You may have noticed that this newsletter is showing up a little bit later than usual, and it’s for good reason: release of the newsletter will now happen after the monthly business meeting so that we can have a chance to keep everybody up to date on the latest information. Sometimes, this will mean the newsletter shows up a couple of days late. But, the upshot is that you’ll now be able to see what we discussed at the recent business meeting and have time to digest it before our general meeting in case you want to give some feedback. Now that we’re on the new format, business meetings (and the oft neglected Light Pollution Committee Meeting), are going to start being open to all members of the club again by simply joining up in the respective chat rooms the Wednesday before the first Monday of the month—which I encourage people to do, especially if you have some ideas you want to see the club put into action.
  • HET Publication Report HET Board Meeting 3/4 December 2020 Zoom Land

    HET Publication Report HET Board Meeting 3/4 December 2020 Zoom Land

    HET Publication Report HET Board Meeting 3/4 December 2020 Zoom Land 1 Executive Summary • There are now 420 peer-reviewed HET publications – Fifteen papers published in 2019 – As of 27 November, nineteen published papers in 2020 • HET papers have 29363 citations – Average of 70, median of 39 citations per paper – H-number of 90 – 81 papers have ≥ 100 citations; 175 have ≥ 50 cites • Wide angle surveys account for 26% of papers and 35% of citations. • Synoptic (e.g., planet searches) and Target of Opportunity (e.g., supernovae and γ-ray bursts) programs have produced 47% of the papers and 47% of the citations, respectively. • Listing of the HET papers (with ADS links) is given at http://personal.psu.edu/dps7/hetpapers.html 2 HET Program Classification Code TypeofProgram Examples 1 ToO Supernovae,Gamma-rayBursts 2 Synoptic Exoplanets,EclipsingBinaries 3 OneorTwoObjects HaloofNGC821 4 Narrow-angle HDF,VirgoCluster 5 Wide-angle BlazarSurvey 6 HETTechnical HETQueue 7 HETDEXTheory DarkEnergywithBAO 8 Other HETOptics Programs also broken down into “Dark Time”, “Light Time”, and “Other”. 3 Peer-reviewed Publications • There are now 420 journal papers that either use HET data or (nine cases) use the HET as the motivation for the paper (e.g., technical papers, theoretical studies). • Except for 2005, approximately 22 HET papers were published each year since 2002 through the shutdown. A record 44 papers were published in 2012. • In 2020 a total of fifteen HET papers appeared; nineteen have been published to date in 2020. • Each HET partner has published at least 14 papers using HET data. • Nineteen papers have been published from NOAO time.
  • Download This Issue (Pdf)

    Download This Issue (Pdf)

    Volume 46 Number 2 JAAVSO 2018 The Journal of the American Association of Variable Star Observers Unmanned Aerial Systems for Variable Star Astronomical Observations The NASA Altair UAV in flight. Also in this issue... • A Study of Pulsation and Fadings in some R CrB Stars • Photometry and Light Curve Modeling of HO Psc and V535 Peg • Singular Spectrum Analysis: S Per and RZ Cas • New Observations, Period and Classification of V552 Cas • Photometry of Fifteen New Variable Sources Discovered by IMSNG 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 Laszlo L. Kiss Ulisse Munari Dunlap Institute of Astronomy Konkoly Observatory INAF/Astronomical Observatory and Astrophysics Budapest, Hungary of Padua and University of Toronto Asiago, Italy Toronto, Ontario, Canada Katrien Kolenberg Universities of Antwerp Karen Pollard Associate Editor and of Leuven, Belgium Director, Mt. John Observatory Elizabeth O. Waagen and Harvard-Smithsonian Center University of Canterbury for Astrophysics Christchurch, New Zealand Production Editor Cambridge, Massachusetts Michael Saladyga Nikolaus Vogt Kristine Larsen Universidad de Valparaiso Department of Geological Sciences, Valparaiso, Chile Editorial Board Central Connecticut State Geoffrey C. Clayton University, Louisiana State University New Britain, Connecticut Baton Rouge, Louisiana Vanessa McBride Kosmas Gazeas IAU Office of Astronomy for University of Athens Development; South African Athens, Greece Astronomical Observatory; and University of Cape Town, South Africa The Council of the American Association of Variable Star Observers 2017–2018 Director Stella Kafka President Kristine Larsen Past President Jennifer L.
  • Uv Ceti Type Variable Stars Presented in the General Catalogue of Variable Stars

    Uv Ceti Type Variable Stars Presented in the General Catalogue of Variable Stars

    IX BULGARIAN-SERBIAN ASTRONOMICAL CONFERENCE: . ASTROINFORMATICS . Sofia, 2 – 4 July, 2014 UV CETI TYPE VARIABLE STARS PRESENTED IN THE GENERAL CATALOGUE OF VARIABLE STARS Katya Tsvetkova Institute of Mathematics and Informatics, Bulgarian Academy of Sciences Sofia, 2 – 4 July, 2014 IX BULGARIAN-SERBIAN ASTRONOMICAL CONFERENCE: . ASTROINFORMATICS . Abstract We present the place and the status of UV Ceti type variable stars in the General Catalogue of Variable Stars (GCVS4, edition April 2013) having in view the improved typological classification, which is accepted in the already prepared GCVS4.2 edition. The improved classification is based on understanding the major astrophysical reasons for variability. The distribution statistics is done on the basis of the data from the GCVS4 and addition of data from the 80th Name List of Variable Stars - altogether 47 967 variable stars with determined type of variability. The class of the eruptive variable stars includes variables showing irregular or semi-regular brightness variations as a consequence of violent processes and flares occurring in their chromospheres and coronae and accompanied by shell events or mass outflow as stellar winds and/or by interaction with the surrounding interstellar matter. In this class the type of the UV Ceti stars is referred together with the types of Irregular variables (Herbig Ae/Be stars; T Tau type stars (classical and weak- line ones), connected with diffuse nebulae, or RW Aurigae type stars without such connection; FU Orionis type; YY Orionis type; Yellow
  • Making a Sky Atlas

    Making a Sky Atlas

    Appendix A Making a Sky Atlas Although a number of very advanced sky atlases are now available in print, none is likely to be ideal for any given task. Published atlases will probably have too few or too many guide stars, too few or too many deep-sky objects plotted in them, wrong- size charts, etc. I found that with MegaStar I could design and make, specifically for my survey, a “just right” personalized atlas. My atlas consists of 108 charts, each about twenty square degrees in size, with guide stars down to magnitude 8.9. I used only the northernmost 78 charts, since I observed the sky only down to –35°. On the charts I plotted only the objects I wanted to observe. In addition I made enlargements of small, overcrowded areas (“quad charts”) as well as separate large-scale charts for the Virgo Galaxy Cluster, the latter with guide stars down to magnitude 11.4. I put the charts in plastic sheet protectors in a three-ring binder, taking them out and plac- ing them on my telescope mount’s clipboard as needed. To find an object I would use the 35 mm finder (except in the Virgo Cluster, where I used the 60 mm as the finder) to point the ensemble of telescopes at the indicated spot among the guide stars. If the object was not seen in the 35 mm, as it usually was not, I would then look in the larger telescopes. If the object was not immediately visible even in the primary telescope – a not uncommon occur- rence due to inexact initial pointing – I would then scan around for it.
  • Newsletter for Iya

    Newsletter for Iya

    IN THIS ISSUE: H FEATURE ARTICLE T UMI: FROM MIRA to ??? GRANT FOSTER . 9 H EYEPIECE VIEWS M . SIMONSEN: AVOIDING BIAS . 10 twINKLE, twINKLE, QUASI-STAR . 11 ISSUE NO.43 JAnuARY 2010 WWW.AAVSO.ORG D . LEVY: SOME MUSINGS ON VARIABLE STARS . 12 H ALSO THE WILLIAM TYLER OLCott TANKARD . 6 LEttER FROM AN OBSERVER . 7 VOLUNTEER SUPERSTARS . 8 Complete table of contents on page 2 LISTEN UP! AAVSO Restless uniVERse THE AAVSO PODCAST Newsletter FOR IYA . 19 SINCE 1911... The AAVSO is an international non-profit organization of variable star observers whose mission is: to observe and analyze variable stars; to collect and archive observations for FROM THE worldwide access; and to forge strong collaborations and mentoring between amateurs and professionals that promote both scientific research DIRECTOR’S DESK and education on variable sources. ARNE A. HENDEN elcome to 2010! I’m happy to reach this fields with CHET error reports, all of the LPV Wmilestone, as it means all of my CCD image legacy stars, all of the RR Lyr legacy stars, new filenames, which are named with yymmdd, now novae, etc. It is amazing to me how fast sequences have a “1” as the first digit rather than a “0”, and can be created with SeqPlot, uploaded to the PRESIDENT’S MESSAGE iraf likes them better (yes, I know that I will have Variable Star comparison Database, and then be a Y2.5K problem). I bet you each have a different immediately available to the observers through JAIME R. GARCIA reason why, or why not, to like the beginning of a the Variable Star Plotter.
  • Milestone Goto-Bino Series .Cdr

    Milestone Goto-Bino Series .Cdr

    Kson MilestoneK Standard Alt/Az GOTO Mount INSTRUCTIONS CONTENT FOR KSON STANDARD ALT/AZ GOTO USER INTRODUCTION.................................................................................1 ACCESSORIES..................................................................................2 ASSEMBLY INSTRUCTIONS.............................................................3 FEATURES.........................................................................5 OPERATION MANUAL FOR SKYTOUCH CONTROLLER............... 6 KEY DESCRIPTION.................................................................................6 STATUS DESCRIPTION...........................................................................6 OPERATION PROCESS...........................................................................7 POWER ON......................................................................................7 WARNING........................................................................................7 ALIGNMENT STATUS........................................................................7 CHANGE THE DATE..................................................................7 CHANGE THE TIME...................................................................8 CHANGE THE SITE...................................................................8 ALIGNMENT.............................................................................9 NAVIGATION STATUS.....................................................................11 MENU STATUS................................................................................11