The thermal-radiative wind in low mass X-ray binary H 1743-322; Radiation hydrodynamic simulations. (arXiv:1905.11763v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Tomaru_R/0/1/0/all/0/1">Ryota Tomaru</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Done_C/0/1/0/all/0/1">Chris Done</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ohsuga_K/0/1/0/all/0/1">Ken Ohsuga</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nomura_M/0/1/0/all/0/1">Mariko Nomura</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Takahashi_T/0/1/0/all/0/1">Tadayuki Takahashi</a>
Blueshifted absorption lines are seen in high inclination black hole binary
systems in their disc dominated states, showing these power an equatorial disc
wind. While some contribution from magnetic winds remain a possibility, thermal
and thermal-radiative winds are expected to be present. We show results from
radiation hydrodynamic simulations which show that the additional radiation
force from atomic features (bound-free and lines) are important along with
electron scattering. Together, these increase the wind velocity at high
inclinations, so that they quantitatively match the observations in H 1743-322,
unlike purely thermal winds which are too slow. We highlight the role played by
shadowing of the outer disc from the (sub grid) inner disc Compton heated
layer, and show that the increase in shadow from the higher Compton temperature
after the spectral transition to the hard state leads to strong suppression of
the wind. Thermal-radiative winds explain all of the spectral features (and
their disappearance) in this simplest wind system and magnetic winds play only
a minor role. We speculate that thermal-radiative winds can explain all the
spectral features seen in the more complex (larger disc size) binaries, GRO
J1655-40 and GRS 1915+105, without requiring magnetic winds.
Blueshifted absorption lines are seen in high inclination black hole binary
systems in their disc dominated states, showing these power an equatorial disc
wind. While some contribution from magnetic winds remain a possibility, thermal
and thermal-radiative winds are expected to be present. We show results from
radiation hydrodynamic simulations which show that the additional radiation
force from atomic features (bound-free and lines) are important along with
electron scattering. Together, these increase the wind velocity at high
inclinations, so that they quantitatively match the observations in H 1743-322,
unlike purely thermal winds which are too slow. We highlight the role played by
shadowing of the outer disc from the (sub grid) inner disc Compton heated
layer, and show that the increase in shadow from the higher Compton temperature
after the spectral transition to the hard state leads to strong suppression of
the wind. Thermal-radiative winds explain all of the spectral features (and
their disappearance) in this simplest wind system and magnetic winds play only
a minor role. We speculate that thermal-radiative winds can explain all the
spectral features seen in the more complex (larger disc size) binaries, GRO
J1655-40 and GRS 1915+105, without requiring magnetic winds.
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