Magnetic Braking at work in binaries. (arXiv:2003.11387v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Rensbergen_W/0/1/0/all/0/1">Walter van Rensbergen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Greve_J/0/1/0/all/0/1">Jean Pierre de Greve</a>
Our binary evolutionary code predicted until now the position of both stars
in the HRD, the characteristics of the accretion disk around the gainer in the
case that there is enough space between both stars for this disk. Our code
includes a complete description of the tidal interaction. The code was now
extended with the action of magnetic braking. Without this phenomenon the
rotational velocity of the gainer can not be predicted.Magnetic braking and
tides act together and the evolution of the equatorial velocity can now be
followed up from birth to death of the binary. From Figure (1) in the text one
sees that the equatorial velocity is kept most of the time far below critical.
When the equatorial velocity is large a magnetic field is created. The
subsequent magnetic braking is applied on a large number of binaries for which
the equatorial velocity is measured. The result is encouraging: a large
fraction of observed equatorial velocities is reproduced by our calculations.
Our binary evolutionary code predicted until now the position of both stars
in the HRD, the characteristics of the accretion disk around the gainer in the
case that there is enough space between both stars for this disk. Our code
includes a complete description of the tidal interaction. The code was now
extended with the action of magnetic braking. Without this phenomenon the
rotational velocity of the gainer can not be predicted.Magnetic braking and
tides act together and the evolution of the equatorial velocity can now be
followed up from birth to death of the binary. From Figure (1) in the text one
sees that the equatorial velocity is kept most of the time far below critical.
When the equatorial velocity is large a magnetic field is created. The
subsequent magnetic braking is applied on a large number of binaries for which
the equatorial velocity is measured. The result is encouraging: a large
fraction of observed equatorial velocities is reproduced by our calculations.
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