Using P-mode Oscillations of Infrared CO Lines to Probe the Solar Atmosphere

Details Using P-mode Oscillations of Infrared CO Lines to Probe the Solar Atmosphere Using P-mode Oscillations of Infrared CO Lines to Probe the Solar Atmosphere

Jan 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21715508c&link_type=abstract

American Astronomical Society, AAS Meeting #217, #155.08; Bulletin of the American Astronomical Society, Vol. 43, 2011

Astronomy and Astrophysics

Astronomy

Scientific paper

Using the 14 m vertical spectrograph on the NSO McMath-Pierce telescope, CO spectra of the Sun are obtained that are centered around 4.6 µm. From these spectra, Gaussian fits are made to the 46664 Å line to acquire velocity, temperature and continuum parameters. With these parameters, full disk maps are made for each. By creating 3-D maps of velocity and temperature, p-mode oscillations are found by taking a power spectrum of both. Variations in power and central frequency with µ for the velocity map are found by taking power spectra at different annuli of µ. It is seen that power increases as µ increases. The next step is to measure the phase difference and coherence between the velocity and temperature maps, which will be presented. These are also found for different values of µ to better understand how CO changes higher in the solar atmosphere.
This work is carried out through the National Solar Observatory Research Experiences for Undergraduate (REU) site program, which is co-funded by the Department of Defense in partnership with the National Science Foundation REU Program. The National Solar Observatory is operated by the Association of Universities for Research in Astronomy, Inc. (AURA) under cooperative agreement with the National Science Foundation.

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