The generalized hardness-intensity diagram for black hole and neutron star X-ray binaries. (arXiv:1909.08932v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Singh_C/0/1/0/all/0/1">Chandra B. Singh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Garofalo_D/0/1/0/all/0/1">David Garofalo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kennedy_K/0/1/0/all/0/1">Kathryn Kennedy</a>
Over the past half century, X-ray and radio observations of accreting neutron
stars and stellar mass black holes have yielded a rich observational picture
with common features including state transitions and jet formation, but also
sharp differences. While black hole X-ray binaries overwhelmingly suppress jets
in so-called soft states, accreting neutron stars are less restrictive, with a
soft state wind observed in some sources to co-exist with a jet. We propose an
explanation for these differences that leads to a generalization of a
foundational element, the hardness-intensity diagram of Fender et al (2004).
The inverse relation between jets and winds fits into a picture that connects
to prograde accretion while the possibility of counterrotation between
accretion disk and compact object accounts for observed differences in
accreting neutron stars. This picture comes with a surprising twist, which is
that neutron stars embody the small-scale analog of FRII quasars, an idea that
allows us to complete the scale invariant picture for the jet-disk connection.
Over the past half century, X-ray and radio observations of accreting neutron
stars and stellar mass black holes have yielded a rich observational picture
with common features including state transitions and jet formation, but also
sharp differences. While black hole X-ray binaries overwhelmingly suppress jets
in so-called soft states, accreting neutron stars are less restrictive, with a
soft state wind observed in some sources to co-exist with a jet. We propose an
explanation for these differences that leads to a generalization of a
foundational element, the hardness-intensity diagram of Fender et al (2004).
The inverse relation between jets and winds fits into a picture that connects
to prograde accretion while the possibility of counterrotation between
accretion disk and compact object accounts for observed differences in
accreting neutron stars. This picture comes with a surprising twist, which is
that neutron stars embody the small-scale analog of FRII quasars, an idea that
allows us to complete the scale invariant picture for the jet-disk connection.
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