Dynamics of hot galactic winds launched from non-uniform starburst cores. (arXiv:2210.07193v1 [astro-ph.GA])

Dynamics of hot galactic winds launched from non-uniform starburst cores. (arXiv:2210.07193v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Nguyen_D/0/1/0/all/0/1">Dustin D. Nguyen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Thompson_T/0/1/0/all/0/1">Todd A. Thompson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schneider_E/0/1/0/all/0/1">Evan E. Schneider</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lopez_S/0/1/0/all/0/1">Sebastian Lopez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lopez_L/0/1/0/all/0/1">Laura A. Lopez</a>

The galactic wind model of Chevalier1985 (CC85) assumes $textit{uniform}$
energy and mass-injection within the starburst galaxy nucleus. However, the
structure of nuclear star clusters, bulges, and star-forming knots are
inherently non-uniform. We generalize to cases with non-uniform energy/mass
injection that scale as $r^{-Delta}$ within the starburst volume $R$,
providing solutions for $Delta = 0$, 1/2, 1, 3/2, and 2. In marked contrast
with the CC85 model ($Delta=0$), which predicts zero velocity at the center,
for a singular isothermal sphere profile ($Delta=2$), we find that the flow
maintains a $textit{constant}$ Mach number of $mathcal{M}=sqrt{3/5} simeq
0.77$ throughout the volume. The fast interior flow can be as $v_{r < R} =
(dot{E}_T/3dot{M}_T)^{1/2} simeq 0.41 , v_infty$, where $v_infty$ is the
asymptotic velocity, and $dot{E}_T$ and $dot{M}_T$ are the total energy and
mass injection rates. For $v_infty simeq 2000 , mathrm{km , s^{-1}}$,
$v_{r<R} simeq 820 , mathrm{km, s^{-1}}$ throughout the wind-driving
region. The temperature and density profiles of the non-uniform models may be
important for interpreting spatially-resolved maps of starburst nuclei. We
compute velocity resolved spectra to contrast the CC85 and $Delta=2$ models.
Next generation X-ray space telescopes such as XRISM may assess these kinematic
predictions.

The galactic wind model of Chevalier1985 (CC85) assumes $textit{uniform}$
energy and mass-injection within the starburst galaxy nucleus. However, the
structure of nuclear star clusters, bulges, and star-forming knots are
inherently non-uniform. We generalize to cases with non-uniform energy/mass
injection that scale as $r^{-Delta}$ within the starburst volume $R$,
providing solutions for $Delta = 0$, 1/2, 1, 3/2, and 2. In marked contrast
with the CC85 model ($Delta=0$), which predicts zero velocity at the center,
for a singular isothermal sphere profile ($Delta=2$), we find that the flow
maintains a $textit{constant}$ Mach number of $mathcal{M}=sqrt{3/5} simeq
0.77$ throughout the volume. The fast interior flow can be as $v_{r < R} =
(dot{E}_T/3dot{M}_T)^{1/2} simeq 0.41 , v_infty$, where $v_infty$ is the
asymptotic velocity, and $dot{E}_T$ and $dot{M}_T$ are the total energy and
mass injection rates. For $v_infty simeq 2000 , mathrm{km , s^{-1}}$,
$v_{r<R} simeq 820 , mathrm{km, s^{-1}}$ throughout the wind-driving
region. The temperature and density profiles of the non-uniform models may be
important for interpreting spatially-resolved maps of starburst nuclei. We
compute velocity resolved spectra to contrast the CC85 and $Delta=2$ models.
Next generation X-ray space telescopes such as XRISM may assess these kinematic
predictions.

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