A distinct shell structure in H I-line-emission at intermediate galactic latitudes

Details A distinct shell structure in H I-line-emission at intermediate galactic latitudes A distinct shell structure in H I-line-emission at intermediate galactic latitudes

Sep 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982a%26a...113..340v&link_type=abstract

Astronomy and Astrophysics, vol. 113, no. 2, Sept. 1982, p. 340-343. Research sponsored by the Deutsche Forschungsgemeinschaft.

Astronomy and Astrophysics

Astrophysics

4

H Lines, Interstellar Gas, Radiation Sources, Supernova Remnants, Emission Spectra, Galactic Rotation, Line Spectra, Milky Way Galaxy, Pulsars, Radio Waves

Scientific paper

The H I shell structure GS 130-22.5, observed with high frequency resolution and satisfactory spatial resolution, is discussed. The distance is about 450 pc, the radius about 24 pc, the expansion velocity about 12.5 km/s, and the shell-gas kinetic temperature about 80 K or less. Kinematical distances determined from different models of galactic rotation are shown. The possibility is considered that the nearby pulsar PSR 0809+74 with known proper motion is associated with the phenomenon and originated in a supernova event. This event must have occurred about a million years ago with an initial energy output of about 10 to the 49th ergs. An attempt is made to show why the shell is not visible in the radio continuum. When free-free emission or synchrotron radiation are considered, the resulting brehmsstrahlung in the radiofrequency range is too small to be detectable. If a supernova created the shell, it must have been a type II explosion.

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