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Excitation of solar p-modes

Goldreich, Peter and Murray, Norman and Kumar, Pawan (1994) Excitation of solar p-modes. Astrophysical Journal, 424 (1). pp. 466-479. ISSN 0004-637X. https://resolver.caltech.edu/CaltechAUTHORS:20130417-140841036

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Abstract

We investigate the rates at which energy is supplied to individual p-modes as a function of their frequencies v and angular degrees ℓ. The observationally determined rates are compared with those calculated on the hypothesis that the modes are stochastically excited by turbulent convection. The observationally determined excitation rate is assumed to be equal to the product of the mode's energy E and its (radian) line width Г. We obtain E from the mode's mean square surface velocity with the aid of its velocity eigenfunction. We assume that Г measures the mode's energy decay rate, even though quasi-elastic scattering may dominate true absorption. At fixed ℓ, EГ rises as v^7 at low v, reaches a peak at v ≈ 3.5 mHz, and then declines as v^(-4•4) at higher v. At fixed v, EГ exhibits a slow decline with increasing ℓ. To calculate energy input rates, P_ α, we rely on the mixing-length model of turbulent convection. We find entropy fluctuations to be about an order of magnitude more effective than the Reynolds stress in exciting p-modes. The calculated P_ α mimic the v^7 dependence of EГ at low v and the v^(-4•4) dependence at high v. The break of 11.4 powers in the v-dependence of EГ across its peak is attributed to a combination of (1) the reflection of high-frequency acoustic waves just below the photosphere where the scale height drops precipitously and (2) the absence of energy-bearing eddies with short enough correlation times to excite high-frequency modes. Two parameters associated with the eddy correlation time are required to match the location and shape of the break. The appropriate values of these parameters, while not unnatural, are poorly constrained by theory. The calculated P_ α can also be made to fit the magnitude of EГ with a reasonable value for the eddy aspect ratio. Our results suggest a possible explanation for the decline of mode energy with increasing ℓ at fixed v. Entropy fluctuations couple to changes in volume associated with the oscillation mode. These decrease with decreasing n at fixed v, becoming almost zero for the ƒ-mode.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1086/173904DOIUNSPECIFIED
http://adsabs.harvard.edu/abs/1994ApJ...424..466GPublisherUNSPECIFIED
Additional Information:© 1994 American Astronomical Society. Received 1993 March 31; accepted 1993 September 16. We are indebted to K. Libbrecht and M. Woodard for sharing their mode amplitudes and line widths with us, and for many informative discussions. We thank Sylvain Korzennik for the use of Figure 5, and M. Rast and G. Willette for useful comments. This research was supported in part by NSF grant AST 89-13664 and NASA grant NAGW 3018.
Funders:
Funding AgencyGrant Number
NSFAST 89-13664
NASANAGW 3018
Subject Keywords:convection; Sun: interior; Sun: oscillations
Issue or Number:1
Record Number:CaltechAUTHORS:20130417-140841036
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20130417-140841036
Official Citation:Excitation of solar p-modes Goldreich, P., Murray, N., & Kumar, P. Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 424, no. 1, p.466-479 Bibliographic Code: 1994ApJ...424..466G
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:37996
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:19 Apr 2013 18:03
Last Modified:03 Oct 2019 04:53

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