Difference between revisions of "Variable Stars"
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*Also, I started a page a bit ago of the Niles West sub-group's effort to observe longer period variables such as Mira-type and Cepheid-type, the latter that Joey alluded to. The Mid-IR group, i.e. us, is looking for variables with even shorter periods, on the order of which we can observe with our several hours long data sets. See "Mr. DeCoster's LPV Material" under one of our sub-headings.<BR> | *Also, I started a page a bit ago of the Niles West sub-group's effort to observe longer period variables such as Mira-type and Cepheid-type, the latter that Joey alluded to. The Mid-IR group, i.e. us, is looking for variables with even shorter periods, on the order of which we can observe with our several hours long data sets. See "Mr. DeCoster's LPV Material" under one of our sub-headings.<BR> | ||
[[image:NITARP-Lyr Cyg Paint-5550-.JPG|600px|thumb|center|Chi Cyg area in Cygnus]] <BR> | [[image:NITARP-Lyr Cyg Paint-5550-.JPG|600px|thumb|center|Chi Cyg area in Cygnus]] <BR> | ||
| − | [[image:Ss_cyg_with_paint.JPG| | + | [[image:Ss_cyg_with_paint.JPG|400px|thumb|center|SS Cyg with Yerkes 24" telescope, 7-29-2010. Mr. D needs HELP with resetting his PAINT program defaults!]] <BR> |
Ss_cyg_with_paint.JPG | Ss_cyg_with_paint.JPG | ||
--[[User:Decoster|Richard DeCoster]] 12:56, 29 July 2010 (PDT) | --[[User:Decoster|Richard DeCoster]] 12:56, 29 July 2010 (PDT) | ||
Revision as of 20:14, 29 July 2010
I already had this on my page, but here's the link to make it more easily accessible. Yes, I know it's Wikipedia, but the information is pretty legitimate. And it is a bit long, but even a scan through can get some good points.
Variable Stars on Wikipedia
The main points I got out of this are:
- Variable stars are classified as either intrinsic or extrinsic. Intrinsic is when the star itself is pulsating or having some sort of eruptions, causing the change in brightness. Extrinsic is when the star's brightness is blocked by another orbiting star.
- Specifically, I think the ones we've been studying are considered cepheids, or variable stars with shorter periods like days or months and their variation isn't very varying (say that five times fast! The site calls their luminosities "regular.")
- Helium is the main cause of cepheids' fluctuations. Ionization, to be exact; gotta love chemistry.
--Joey Romero 19:12, 24 July 2010 (PDT)
You Rock Joey! So if we are looking fore these rapidly varying stars in this study, why might it be useful to look at these in the infrared range? Mr DeCoster is a variable star groupie, so I hope he chimes in here! Don't forget the link that someone posted on the previous page http://aavso.org/vstar/ that has lots more info. --Peggy Piper 20:08, 25 July 2010 (PDT)
AAVSO recently greatly modified [?improved] its web page. I am still trying to recoup.
- We took some pictures at Yerkes last night of one of the more famous variable stars SS Cygni. I'll try to post one such picture.
- Also, I started a page a bit ago of the Niles West sub-group's effort to observe longer period variables such as Mira-type and Cepheid-type, the latter that Joey alluded to. The Mid-IR group, i.e. us, is looking for variables with even shorter periods, on the order of which we can observe with our several hours long data sets. See "Mr. DeCoster's LPV Material" under one of our sub-headings.
Ss_cyg_with_paint.JPG --Richard DeCoster 12:56, 29 July 2010 (PDT)
