Sign on

SAO/NASA ADS Astronomy Abstract Service

· Find Similar Abstracts (with default settings below)
· Electronic Refereed Journal Article (HTML)
· Full Refereed Journal Article (PDF/Postscript)
· References in the article
· Citations to the Article (64) (Citation History)
· Refereed Citations to the Article
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
How to Channel Photospheric Oscillations into the Corona
Authors:
De Pontieu, B.; Erdélyi, R.; De Moortel, I.
Affiliation:
AA(Lockheed Martin Solar and Astrophysics Lab, Org. ADBS, Building 252, 3251 Hanover Street, Palo Alto, CA 94304; ), AB(Solar Physics and Upper Atmosphere Research Group, University of Sheffield, Hicks Building, Hounsfield Road, Sheffield S3 7RH, England, UK; ), AC(School of Mathematics and Statistics, University of St. Andrews, North Haugh, St. Andrews KY16 9SS, Scotland, UK; )
Publication:
The Astrophysical Journal, Volume 624, Issue 1, pp. L61-L64. (ApJL Homepage)
Publication Date:
05/2005
Origin:
UCP
ApJ Keywords:
Magnetic Fields, Sun: Chromosphere, Sun: Corona, Sun: Photosphere, Sun: Transition Region
DOI:
10.1086/430345
Bibliographic Code:
2005ApJ...624L..61D

Abstract

There are now many observations of waves in the solar corona with periods around 5 minutes. The source of these waves is uncertain, although global p-modes in the photosphere are an obvious candidate, given the similarity of the dominant periods. However, p-modes are traditionally considered evanescent in the upper photosphere, and it has been unclear how they could propagate through the chromosphere into the corona. Using a numerical model, we show that photospheric oscillations with periods around 5 minutes can actually propagate into the corona so long as they are guided along an inclined magnetic flux tube. The nonverticality of the flux tube increases the acoustic cutoff period to values closer to the dominant periods of the photospheric oscillations, thus allowing tunneling or even direct propagation into the outer atmosphere. The photospheric oscillations develop into shocks, which drive chromospheric spicules and reach the corona. We suggest that Transition Region and Coronal Explorer (TRACE) observations of propagating magnetoacoustic waves in the corona represent these shocked and tunneled photospheric oscillations. We also explore how seismology of these waves could be exploited to determine the connectivity between photosphere and corona.
Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)
   

Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints