Wave Propagation in a Magnetized Atmosphere

Details Wave Propagation in a Magnetized Atmosphere Wave Propagation in a Magnetized Atmosphere

May 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sh41a01b&link_type=abstract

American Geophysical Union, Spring Meeting 2001, abstract #SH41A-01

Computer Science

Sound

7507 Chromosphere, 7522 Helioseismology, 7524 Magnetic Fields, 7529 Photosphere, 7546 Transition Region

Scientific paper

Numerical simulations of MHD wave propagation in plane-parallel atmospheres threaded by non-trivial potential magnetic fields will be presented, and their implications for understanding distinctions between intranetwork and internetwork oscillations will be discussed. Our findings basically confirm the conjecture of McIntosh et al. (2001, ApJ 548, L237), that the two-dimensional surface where the Alfvén and sound speeds coincide (i.e., where the plasma-β , the ratio of gas to magnetic pressure, is of order unity) plays a fundamental role in mediating the conversion between the fast-, intermediate- (Alfvén), and slow-Magneto-Atmospheric-Gravity (MAG) waves. For example, upward-propagating acoustic waves generated at the base of the internetwork photosphere suffer significant downward reflection when they encounter this β ≈ 1 surface. Close to the network, this surface descends from the upper chromosphere and low corona (which pertains in the internetwork cell interiors) down into the photosphere, and so chromospheric oscillation `shadows' are predicted to surround the network. In the network, strong vertical magnetic fields further depress the β ≈ 1 surface below the surface layers where the (magnetic field-aligned) acoustic waves (i.e., slow MAG-waves) are generated. For frequencies in excess of the cutoff frequency, these acoustic waves suffer little reflection from the overlying atmosphere and they steepen as they progress upward.

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