Témata z oblasti zákrytových dvojhvězd
Vedoucí/školitel: Miloslav Zejda
O-C database with analytical tools O-C databáze s analytickými nástroji
Near contact binaries Takřka dotykové dvojhvězdy
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Determination of distance using W UMa binaries Určení vzdálenosti pomocí hvězd typu W UMa
And others ...
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Phase
0-C database with analytical tools O-C databáze s analytickými nástroji
The most common tools for studying eclipsing binaries:
• light/phase curve,
• radial velocity curve,
• O-C diagram (display the development of differencies between observed and calculated/predicted timings of minima)
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Aim:
❖ management of database of minima timings (O-C)
tools for calculations of fit of O-C curves, subtracting fits, calculations of new ephemeris, prediction of future behaviour
❖
0.00 -0.07
AT Peg
+ vis (246)
* PS (17) O pe (26)
• ccd (40) — model
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Epoch
Can be used for TTVs at exoplanets!
Near contact binaries Takřka dotykové dvojhvězdy
kind of close binaries with both components filling or nearly filling their critical
Roche Lobe (Shaw 1990) - two subclasses
Importance:
• NCBs = close binaries in a key evolutionary stage; intermediate objects between the stage of detached and contact systems
• Large temperature difference between the two components while contact in geometry => proof of the TRO
• And others
VIOIO OPH
Aim:
-0.30
❖
❖
Photometric (&spectroscopic) study Determination of parameters, evolutionary status
(CCD+B) (CCD+v) (CCD+PJ -0.10 - CCD+I)
0.10
0.50
1.10
1.50
Phased with elements 2455758.3547 + 0.66142613 * E qooo
1.70			
1.90	i       i       i       i       i i	current time (10:01 UTC) i       i       i       i       i       i       i       i i	current time
0.1   0.2   0.3   0.4   0.5   0.6   0.7   0.6   0.9   1.0   1.1   1.2   1.3   1.4   1.5   1.6   1.7   1.8   1.9 2.0
Determination of distance using W UMa binaries Určení vzdálenosti pomocí hvězd typu W UMa
Close binaries include more massive early-type systems and less massive late-type systems— commonly known as W UMa (W Ursae Majoris) type binaries
Based on 27 000 W UMas and GAIA DR1 data - the determination accuracy 8 %
Aim:
-0.6   -0.55    -0.5    -0.45    -0.4   -0.35    -0.3 -0.25 log P [d]
-0.6   -0.55    -0.5    -0.45    -0.4   -0.35   -0.3 -0.25 log P [d]
Using GAIA DR3 data select CBs, and WUMas
Determinate parameters of (orbital) period-luminosity relations (PLRs) Study of possible chcnges of PLRs in different parts of our Galaxy (more brighter (longer-period) W UMas are found in younger environments....)
-0,6   -0.55   -0.5    -0,45    -0,4   -0,35    -0.3 -0.25 1"E P [d]
-0.6   -0.55    -0,5    -0,45    -0.4   -0.35    -0.3 -0.25 l«g P [d]
-0.6   -0.55   -0.5    -0.45    -0.4   -0.35    -0.3 -0.25 log P [d]
-0.6   -0.55    -0.5    -0.45    -0.4   -0.35   -0.3 -0.25 log P [d]
^0.6   -0.55   -0.5    -0.45    -0.4   -0.35    -0.3 -0.25 log P [d]
-0.6   -0.55    -0.5    -0.45    -0.4   -0.35    -0.3 -0.25 log P [d]
Chen et al. 2018