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Name
  GSC 08174-00876  
AAVSO UID
000-BFS-985 (3051 observations)  
Constellation
Vela Sequence
J2000.0
09 12 52.50 -49 10 40.6  (138.21875 -49.17794) Search nearby
B1950.0 09 11 10.36 -48 58 15.6
Proper motion
RA: -5.046 +/- 0.536 mas/yDec: -1.392 +/- 0.500 mas/ySource: Gaia DR1
Galactic coord. 270.714 -0.480
Other names

(Internal only)
2MASS J09125251-4910394 HD 79512 UCAC2 10590497
USNO-B1.0 0408-0140880 VSX J091252.5-491040  
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Variability type
DSCTC
Spectral type A3V - A6V
Mag. range
8.58 - 8.64 V
Discoverer Sebastian Otero, Giorgio Di Scala
Epoch
--
Outburst --
Period 0.075: d  (108 min)
Rise/eclipse dur. --
Remarks
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References
There are currently no additional references filed for this star.
External Links
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Location    Go   
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Catalog Data
Information from selected catalogs obtained by cross-matching to 2 arc seconds using the CDS X-Match Service. These data may not be complete.
2MASS J = 8.07H = 7.95K = 7.88J - K = 0.19
AllWISE W1 = 7.84W2 = 7.88W3 = 7.88W4 = 7.67W1 - W2 = -0.04W3 - W4 = 0.21
APASS-DR9 B = 8.80V = 8.60g' = 9.72r' = 8.61B - V = 0.20
Images
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Size 5' x 5' (297 x 298 pixels)
Center 09 12 52.50 -49 10 40.6 (J2000)
Source STScI
Survey

Red, all sky, 1.0 arcsec/pixel
  Negative
Supporting Documents
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2 DATA FILE 26-1-2008 Di Scala, Giorgio 2008-02-03 11:59 UTC Processed data for HD 79512: 26-1-2008 (UT) Star has displayed multi - periodicity
1 V photometry graph of HD 79512 Di Scala, Giorgio 2008-02-03 11:59 UTC Graph of the data uploaded in file 1.
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Revision History
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1 Di Scala, Giorgio 2008-02-03 16:09 UTC Sebastian Otero originally detected HD 79512 as a possible variable while datamining the ASAS. The data qualiity of the ASAS data was poor. He suspected that it was an EA type. He referred the star to me. I observed it on 3 seperate occasions. The second night's data has been uploaded. It is clearly not EA but a multiperiodic DSCT. Due to its low amplitude, a DSCTC classification is likely. B-V = 0.26 further supporting its DSTC classification. A possibe period of 0.075 days is present. However, a number of other interfering periods are also present and the star needs further observing before these can be identified.

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