Interstellar Mass Outflow to Galactic Halos by the Supernova-driven Parker Instability

Details Interstellar Mass Outflow to Galactic Halos by the Supernova-driven Parker Instability Interstellar Mass Outflow to Galactic Halos by the Supernova-driven Parker Instability

Feb 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996apj...458l..25k&link_type=abstract

Astrophysical Journal Letters v.458, p.L25

Astronomy and Astrophysics

Astronomy

26

Ism: Bubbles, Ism: Magnetic Fields, Ism: Supernova Remnants, Magnetohydrodynamics: Mhd

Scientific paper

We here demonstrate by means of two-dimensional magnetohydrodynamic simulations that even a single supernova (SN) explosion can easily trigger a Parker instability. When SNs occur in the galactic disk with horizontal magnetic fields, an outgoing blast wave will lift up the fields, thus forming an Omega -shaped field structure. Hence, the interstellar medium (ISM) can effectively be confined inside the Omega -shaped, bent fields because of their decelerating J{X}B force. It is thus usually thought that unless unrealistically large numbers of SNs occur, it is difficult for the ISM to blow out into the halo. We find, however, that this is the case only before the Parker instability is excited; namely, for the first several megayears after the explosion. The gas frozen into the Omega -shaped magnetic fields will eventually slide down along the fields to the galactic disk by gravity, so the magnetic fields can move upward by an enhanced magnetic buoyancy. In roughly tens of megayears after the explosions the Parker instability will be triggered, giving rise to a blowout of the disk material into the halo. Importantly, a nonlinear Parker instability can be triggered quite generally; i.e., even when the underlying gas layer is stable against infinitesimal perturbations.

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