Epsilon Aurigae Eclipse Campaign 2009

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From Robin Leadbeater

The eclipsing object is still very clear spectroscopically in the K 7699A and Na D lines.

During photometric egress, the Equivalent Width of the K 7699A line reduced mainly through narrowing of the line, with the line core intensity staying strong (see the recent campaign newsletter 23)

http://www.hposoft.com/EAur09/NL09/NL23.pdf

Now, after photometric 4th contact the narrowing has stopped and the EW is reducing because the overall line strength is now dropping. This suggests either the absorbing "atmosphere" is less dense or it is covering less of the F star.

If we look at the sodium D lines though (taken by Olivier Thizy during the OHP workshop), we find that the absorption in core of the Na D lines after removing the outside eclipse component is still 90% so we know that the atmosphere must still be effectively completely covering the F star.

This suggests that the K/Na atmosphere is currently getting less dense rather than reducing in extent. This may be consistent with the recent "flared disc" model EFFECTS OF DUST ON LIGHT CURVES OF EPSILON AURIGAE TYPE LIGHT CURVE J. Budaj, Astronomical Institute of the Slovak Academy of Sciences http://arxiv.org/abs/1107.3517

There are several more months of eclipsing object atmosphere to see before we lose sight of it for another 25 years so continued spectroscopy is needed.

Robin

K I Line Profiles

Na D Line Profiles


International Epsilon Aurigae Campaign 2009 This web site was created by Jeffrey L. Hopkins and Dr. Robert E. Stencel in May of 2006. It is acting as the International Epsilon Aurigae Campaign Web site for the 2009 - 2011 eclipse of the star system. The periodic Campaign Newsletters are edited by Jeffrey Hopkins with Dr. Robert Stencel and Robin Leadbeater as Coeditors. The site is hosted and maintained by the Hopkins Phoenix Observatory. The Eclipse is over! Final Newsletter #24 Now Available! Complete UBVRcIcJH Band Photometric Analysis of 2009-2011 Eclipse Images of all Analysis Plots
			Epsilon Aurigae Star System The epsilon Aurigae system is among the most interesting eclipsing star systems. It has puzzled astronomers for nearly 200 years. It is a bright star (3rd magnitude) located about 3 degrees southwest of Capella and eclipses once every 27.1 years. It is at the vertex of a triangular group of stars known as "The Kids". Zeta Aurigae, another interesting long-period eclipsing binary, makes up one of the other two stars. What makes this star system so intriguing is not just its long period but the length of its eclipse, what happens during the eclipse and what happens out-of-eclipse. The eclipse lasts nearly two years which with the 27.1 year period means the eclipsing body must be gigantic. There have been no satisfactory explanations for this. To make matters even more interesting, there seems to be a mid-eclipse brightening. How can this be? One explanation, according to James Kemp, is that the eclipsing body is a giant cloud of gas enclosing two small stars in orbit around each other. These stars sweep out an area in the middle. It would be a bit like a giant donut. This donut must be tilted such that as it eclipses the primary star, the system's total light decreases and the "donut-hole" allows some of the primary star's light to sneak through at mid-eclipse. To try to unravel this system's mystery, a concentrated effort was undertaken during the 1982-1984 eclipse. Hundreds of astronomers, amateurs and professionals, from around the world, observed the eclipse. Space born satellites observed in the ultraviolet and infrared. Ground based observations were photometric, spectroscopic, and polarmetric. Photometric observations were made with UBV filters, narrow band filters, and at wavelengths into the far infrared. Despite the concentrated efforts, epsilon Aurigae remains a mystery. The secondary eclipse was due to occur around 1996/1997. Detection of the secondary eclipse light variation is on the order of the out-of-eclipse variations. This makes separating the two periods very difficult. An effort is underway to try to predict the pulsations through continuing observations. If these pulsations can be predicted, observation of the secondary eclipse may be possible. For those astronomers (both professional and amateur) interested, while the next eclipse will not start until August of 2009, now will be a good time to join a campaign and get prepared. Also, more out-of-eclipse observations are needed before the next eclipse. Epsilon Aurigae is anything but quiet out-of-eclipse. A seasonal 68 day period that seems to be gradually increasing in amplitude is being seen. There are many surprised yet to be found with this interesting star system. Surely, by the end of the next eclipse, astronomy will have unraveled the mystery of epsilon Aurigae. The History and Evolution of the Disk theory for Epsilon Aurigae
INDEX * Basic System Data Star Chart Star Information * Campaign Members How to Join How to Contribute Member List * 2009 - 2011 Campaign Newsletter #1 Newsletter #2 Newsletter #3 Newsletter #4 Newsletter #5 Newsletter #6 Newsletter #7 Newsletter #8 Newsletter #9 Newsletter #10 Newsletter #11 Newsletter #12 Newsletter #13 Newsletter #14 Newsletter #15 Newsletter #16 Newsletter #17 Newsletter #18 Newsletter #19 Newsletter #20 Newsletter #21 Newsletter #22 Newsletter #23 Newsletter #24 New Final Newsletter Index New * Photometry UBVRIJH Photometry Data Observers DSLR How To Plots Archives References * Spectroscopy New Robin Leadbeater is now handling the submission of Spectroscopic Data High Resolution Low Resolution Observers How To Spectra Line Profiles Archives References * Polarimetry Basics - TBD How To - TBD Data - TBD * References 1982 - 1984 Campaign Newsletters NASA Reference 2384 (.pdf 4.9 MB) Current References Interpretation Resources IBVS Articles History * Similar Star Systems BM Orionis Zeta Aurigae EE Cephei VV Cephei * Links Book Epsilon Aurigae A Mysterious Star System Sold Out! Watch for second edition AAS Poster Paper January 2010 Epsilon Aurigae Two Year Totality Transpiring Images from the 2010 SAS Symposium Big Bear, California 11-13 May 2010 Astronomical Time It is very important that anyone who makes astronomical observations understands astronomical time Mount Wilson/CHARA Trip 21-23 September 2010 Images Mount Hopkins MMT Trip 20-23 December 2010 Images 217 AAS Meeting Report 21 January 2011
		Summary of 1982 - 1984 Eclipse Current 2009 Eclipse Predictions Sign up for the latest on epsilon Aurigae Epsilon Aurigae News List http://tech.groups.yahoo.com/group/EpsilonAurigae
				2009/11 Composite Photometric Plots UB, V, RI & JH Bands as of 08 August 2011 Pre-Ingress. Ingress, Totality and Egress V Band Composite Plot B and U Band Composite Plots R and I Band Composite Plots J and H Band Composite Plots All UBVRIJH Data Archive August 2009 Workshops Created and Presented by Jeffrey L. Hopkins Hopkins Phoenix Observatory DSLR Photometry (ppt 4 MB) DSLR Photometry (pdf 1.4 MB) Spectroscopy (ppt 8.9 MB) Spectroscopy ( pdf 2.5 MB) Recent (04 February 2011) hydrogen alpha Spectra by Jose Ribeiro From Robin Leadbeater The below is an updated graph of total EW of the K 7699A line. The corresponding data points from last eclipse (Lambert and Sawyer) are very sparse around this time but the latest observation here at Three Hills coincides with one of them and agrees in magnitude. The next 2 L&S points (corresponding this eclipse to 26th September and 19th October 2011) hint at step in the curve. It will be interesting to see if a step is seen at the same point this eclipse. Robin EW Plot of KI Line
		Article The Very Long Mystery of Epsilon Aurigae Robert E. Stencel Sky & Telescope, May 2009 Page 58 ********************************* SAS 2009 Papers Epsilon Aurigae, 2009: The eclipse begins observing campaign status (.pdf) Epsilon Aurigae Hydrogen Alpha Emission Line Variation The Horn Dance (.pdf New! SAS 2010 Papers** Epsilon Aurigae Eclipse 2009 - Ingress (.pdf) Epsilon Aurigae Eclipse 2009 - Ingress (.ppt)

	NEW SPECTROSCOPY BOOK *Small Telescope Astronomical Spectroscopy* 240 pages SC full color with CD ROM NOW SHIPPING See: http://www.hposoft.com/SB/SpectroBook.html ***************************************************************************************************** From Robin Leadbeater The eclipsing object is still very clear spectroscopically in the K 7699A and Na D lines. During photometric egress, the Equivalent Width of the K 7699A line reduced mainly through narrowing of the line, with the line core intensity staying strong (see the recent campaign newsletter 23) http://www.hposoft.com/EAur09/NL09/NL23.pdf Now, after photometric 4th contact the narrowing has stopped and the EW is reducing because the overall line strength is now dropping. This suggests either the absorbing "atmosphere" is less dense or it is covering less of the F star. If we look at the sodium D lines though (taken by Olivier Thizy during the OHP workshop), we find that the absorption in core of the Na D lines after removing the outside eclipse component is still 90% so we know that the atmosphere must still be effectively completely covering the F star. This suggests that the K/Na atmosphere is currently getting less dense rather than reducing in extent. This may be consistent with the recent "flared disc" model EFFECTS OF DUST ON LIGHT CURVES OF EPSILON AURIGAE TYPE LIGHT CURVE J. Budaj, Astronomical Institute of the Slovak Academy of Sciences http://arxiv.org/abs/1107.3517 There are several more months of eclipsing object atmosphere to see before we lose sight of it for another 25 years so continued spectroscopy is needed. Robin K I Line Profiles Na D Line Profiles
Epsilon Aurigae Star System Schematic Diagram
Created: 30 May 2006 Modified : 20 April 2012 Web page background artwork by D. Egge (c)1985, with permission Webmaster: HPO SOFT