AAS 200th meeting, Albuquerque, NM, June 2002
Session 53. Structure and Dynamics of Chromospheres
SPD Topical Session Oral, Wednesday, June 5, 2002, 8:30-10:00am, 10:45am-12:30pm, Ballroom B

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[53.01] Stellar Chromospheres and the Sun

M. Giampapa (NSO)

Observations combined with the development of semi-empirical models show that stellar chromospheres and the solar chromosphere share many of the same features. Nevertheless, are homogeneous, single-component models of stellar chromospheres adequate representations of their atmospheres in the light of observations that clearly indicate the multi-component natures of both the solar and stellar chromospheres? Is the distinction between "active" and "quiet" chromosphere stars mainly due to the fractional area coverage of otherwise identical magnetic active regions on their surfaces, or can the distinction be attributed primarily to differing heating rates in a relatively homogeneous atmosphere? Can single-component, static models successfully account for the levels of emission in the dominant radiative coolants in stellar chromospheres? How does the radiative energy balance between the chromosphere and corona change with effective temperature and gravity in the cool half of the H-R diagram? Is there evidence for "cool chromospheres" in main sequence stars? These issues will be addressed in an effort to compare and contrast stellar chromospheres with that of the Sun.

The National Solar Observatory is operated for the National Science Foundation by the Association of Universities for Research in Astronomy.

The author(s) of this abstract have provided an email address for comments about the abstract: giampapa@noao.edu

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Bulletin of the American Astronomical Society, 34
© 2002. The American Astronomical Soceity.