Slingshot prominence evolution for a solar-like star. (arXiv:1902.07545v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+DAngelo_C/0/1/0/all/0/1">Carolina Villarreal D'Angelo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jardine_M/0/1/0/all/0/1">Moira Jardine</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Johnstone_C/0/1/0/all/0/1">Colin P. Johnstone</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+See_V/0/1/0/all/0/1">Victor See</a>
Although the present-day Sun rotates too slowly to exhibit
centrifugally-supported ‘slingshot prominences’, at some time during its past
it may have formed these clouds of cool gas and ejected them into the
interplanetary medium. We determine the time period for this behaviour by using
a rotation evolution code to derive the properties of the formation and
ejection of slingshot prominences during the lifetime of a star similar to our
Sun. The mass, mass loss rate and rate of ejection of these prominences are
calculated using the analytical expression derived in our previous work. We
find that for stars with an initial rotation rate larger than $4.6,
Omega_odot$, about half of all solar mass stars, slingshot prominences will
be present even after the star reaches the main sequence phase. In a fast
rotator, this means that prominences can form until the star reaches $sim 800$
Myr old. Our results also indicate that the mass and lifetime of this type of
prominence have maximum values when the star reaches the ZAMS at an age of
$sim 40$ Myr for a solar mass star.
Although the present-day Sun rotates too slowly to exhibit
centrifugally-supported ‘slingshot prominences’, at some time during its past
it may have formed these clouds of cool gas and ejected them into the
interplanetary medium. We determine the time period for this behaviour by using
a rotation evolution code to derive the properties of the formation and
ejection of slingshot prominences during the lifetime of a star similar to our
Sun. The mass, mass loss rate and rate of ejection of these prominences are
calculated using the analytical expression derived in our previous work. We
find that for stars with an initial rotation rate larger than $4.6,
Omega_odot$, about half of all solar mass stars, slingshot prominences will
be present even after the star reaches the main sequence phase. In a fast
rotator, this means that prominences can form until the star reaches $sim 800$
Myr old. Our results also indicate that the mass and lifetime of this type of
prominence have maximum values when the star reaches the ZAMS at an age of
$sim 40$ Myr for a solar mass star.
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