Other
Scientific paper
May 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21641002s&link_type=abstract
American Astronomical Society, AAS Meeting #216, #410.02; Bulletin of the American Astronomical Society, Vol. 41, p.817
Other
Scientific paper
Magnetohydrodynamic (MHD) turbulence in the solar wind has been extensively studied with in-situ measurements, and many of its characteristics are theoretically understood. It is reasonable to assume that these properties also describe turbulence in other astrophysical plasmas. The Very Local Interstellar Medium consists of the Local Cavity, which contains a number of small clouds in the immediate vicinity of the Sun. The plasma diagnostics of these clouds are quite good, due to very high resolution spectroscopic measurements of interstellar absorption lines in the spectra of nearby stars. These observations allow accurate measurements of line widths. Spectral line widths from lines of several atoms or ions allow separation of the line width into a thermal component and a Doppler width attributable to unresolved, turbulent motions. We are analyzing data on about 30 lines of sight to determine the degree to which this local cloud turbulence resembles, or differs from solar wind turbulence. Topics of particular interest to us are the degree to which the turbulent magnetic field and velocity fluctuations are transverse to a large scale magnetic field extending over tens of parsecs, and whether ions with larger Larmor radii are preferentially heated through interaction with this turbulence. These characteristics are distinctive features of solar wind turbulence. We will also discuss how data from the recently serviced Hubble Space Telescope will advance these investigations and present a clearer view of turbulence in local clouds.
Redfield Seth
Savage Allison H.
Spangler Steven R.
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