YZ Boo


IMAGE DETAILS

Object ............................................ YZ Boo
Constellation ..............................  Bootes
V. Magnitude + Variability......  10.30 - 10.80 / δ Scu

RA / DEC ..................................... 15h:24m.07sec / +36 52m.00sec
Period ...........................................  0.10409156  days

Comparison star .........................  GSC 2569:1184
Check star .................................... G
SC 2569:1050

Date + Time ................................   6/5/2011 - 19:30 UTC
Location .................................... 
"Nunki Observatory" - Skiathos
Optics .........................................   Celestron C 11 HD
Tools ..........................................   CCDsoft
Camera ......................................  
SBIG ST 10 XE
Exposure Time.......................     Red: 2.5  Hours
Mount .......................................   Paramount ME
Guiding ....................................   Unguided
Processing Details ................    Maxim , CCDsoft , AIP4WIN
Notes ........................................   Weather: 8/10 Transparence: 4/6 Humidity : 80 %
Sky Temprature.......................   -10 οC
More Details ...........................    Environment Temperature : 20 oC Camera Temperature - 1.5 οC
Moon Illumination ...............    11%

Target details .........................  
A Delta Scuti variable (sometimes termed dwarf cepheid) is a variable star which exhibits variations in its luminosity due to both radial and non-radial pulsations of the star's surface. Typical brightness fluctuations are from 0.003 to 0.9 magnitudes in V over a period of a few hours, although the amplitude and period of the fluctuations can vary greatly. The stars are usually A0 to F5 type giant or main sequence stars. The high-amplitude Delta Scuti variables are also called AI Velorum stars. They are the second most abundant variable source in the Milky Way after white dwarfs.The variability of period and amplitude of the high-amplitude δ Scuti star YZ Boo was thoroughly investigated by scientists based on a comprehensive analysis of new time-series photometry and other available data


 

Nikos Paschalis