modeling of interacting binary systems

MODELING OF INTERACTING BINARY SYSTEMS

O. Latković, G. Đurašević, I. Vince & A. ČekiAstronomical Observatory of Belgrade

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BINARY STAR RESEARCH IN THE STELLAR PHYSICS GROUP AT AOB

Massive binaries Overcontact systems Systems with gas streams and accretion disks Double-periodic variables

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THE MODEL OF A CLOSE BINARY SYSTEM Roche model

Gravity darkening Irradiation feedback Bright or dark circular

spots

Accretion disk Trapezoid cross-section Radial temperature

distribution Active regions as bright

spots

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ACTIVE REGIONS ON THE DISK: HOT SPOT AND SPIRAL STRUCTURE The HOT SPOT (hot line)

is a representation of the area where the gas stream from the donor impacts the disk around the gainer

The BRIGHT SPOTS represent the brightness irregularities that arise from spiral structure

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V455 CYG: A PECULIAR MASSIVE BINARY WITH AN ACCRETION DISK

Spectroscopy Echelle spectrograph attached to 1.25 m

telescope (SAI Crimean Observatory) Photometry

60 cm telescope (Maidanak Observatory) 60 cm telescope (SAI Crimean Observatory)

System parameters:

Monthly Notices of the Royal Astronomical SocietyVolume 420, Issue 4, pages 3081-3090, 10 FEB 2012 DOI: 10.1111/j.1365-2966.2011.20208.xhttp://onlinelibrary.wiley.com/doi/10.1111/j.1365-2966.2011.20208.x/full#f3

Primary Secondary DiskM[Mʘ] 14.0 5.5R [Rʘ] 6.6 14.4 14.5T [K] 25400 13200 9500

Orbital parametersPORB [d] 8.76aORB [Rʘ] 48.0i [⁰] 78.2

http://onlinelibrary.wiley.com/doi/10.1111/mnr.2012.420.issue-4/issuetoc

http://onlinelibrary.wiley.com/doi/10.1111/j.1365-2966.2011.20208.x/full

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System parameters:



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System parameters:



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System parameters:



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V393 SCO: A DOUBLE-PERIODIC BINARY Observations

REM 60 cm telescope (La Silla) ASAS array (Las Campanas)




PLONG [d] 253 PLONG/PORB 33



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V393 SCO: A DOUBLE-PERIODIC BINARY


Observations REM 60 cm telescope (La Silla) ASAS array (Las Campanas)



PLONG [d] 253 PLONG/PORB 33



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AU MON: ANOTHER DOUBLE-PERIODIC BINARY

Monthly Notices of the Royal Astronomical SocietyVolume 409, Issue 1, pages 329-336, 17 AUG 2010 DOI: 10.1111/j.1365-2966.2010.17310.xhttp://onlinelibrary.wiley.com/doi/10.1111/j.1365-2966.2010.17310.x/full#f1

Primary Secondary DiskM[Mʘ] 7.0 1.20

R [Rʘ] 5.1 10.1 14.5

T [K] 15900 5750 9500

Orbital parametersPORB [d] 11.11

aORB [Rʘ] 42.1

i [⁰] 80.1

PLONG [d] 417 PLONG/PORB 37.5



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RECENT IMPROVEMENTS OF THE MODEL

A different geometrical approach Simultaneous fitting of light and radial velocity curves Elliptical orbits Enhanced modeling of accretion disks Modeling of stellar pulsations

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A DIFFERENT GEOMETRICAL REPRESENTATION Sampling strategy: geodesic grid

Uniform sampling of the surface Allows for very fine division

Colors represent the temperature distribution

Gravity darkening Irradiation feedback

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A DIFFERENT GEOMETRICAL REPRESENTATIONDetailed modeling of the eclipse using adaptive subdivision

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IMPROVED MODELING OF THE ACCRETION DISK

Disk shapes Concave and convex disks Toroidal disks Multiple disks / disks with holes

Fine surface division Temperature distribution and

angular velocity distribution as arbitrary functions

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MODELING OF STELLAR PULSATIONS Perturbations are modeled as spherical harmonics and

applied to position and temperature Arbitrary number of modes Arbitrary pulsation axis

L=4, M=2 L=5, M=5 Superposition

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MODELING OF STELLAR PULSATIONSA single L=10, M=5 mode with exaggerated displacement amplitude

MODELING OF INTERACTING BINARY SYSTEMS

O. Latković, G. Đurašević, I. Vince & A. ČekiAstronomical Observatory of Belgrade

modeling of interacting binary systems

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