EDP Sciences
Free access
Issue
A&A
Volume 378, Number 3, November II 2001
Page(s) 1037 - 1045
Section The Sun
DOI http://dx.doi.org/10.1051/0004-6361:20010569


A&A 378, 1037-1045 (2001)
DOI: 10.1051/0004-6361:20010569

A multi-wavelength study of solar coronal-hole regions showing radio enhancements

T. Moran1, N. Gopalswamy1, I. E. Dammasch2 and K. Wilhelm2

1  Center for Solar Physics and Space Weather, The Catholic University of America, Washington, DC 20064 and NASA Goddard Space Flight Center, Code 682.3, Greenbelt, MD 20771, USA
2  Max-Planck-Institut für Aeronomie, Max-Planck-Str. 2, 37191 Katlenburg-Lindau, Germany

(Received 8 January 2001 / Accepted 9 April 2001 )

Abstract
We observed 17 GHz microwave-enhanced regions in equatorial coronal holes (ECH) together with extreme-ultraviolet (EUV), far-ultraviolet (FUV) and visible emissions in a search for temperature increases which might explain the bright spots in radio wavelengths. The ultraviolet (UV) observations span a wide range of formation temperatures (8000 K to 630 000 K). Increased UV emission was observed at the approximate location of the radio enhancements, but unlike the radio brightening, the UV emission did not exceed the mean quiet sun level. However, there were two observations showing increased H$\alpha$ brightness in radio enhancements above mean quiet sun levels. No H$\alpha$ bright spots were detected in ECHs outside of radio enhancement regions. The ECH H$\alpha$ bright spots were caused by bright fibrils, bright points and a lack of dark fibrils. Since the 17 GHz and H$\alpha$ enhancements are co-spatial, have equal integrated normalized enhanced emission and brightness temperatures, the observations suggest that the radio enhancements are caused by increased fibril radio emission. In addition, increased Fe XII EUV emission was recorded at the location of some well-defined radio enhancements, which were the bases of coronal plumes. Since the radio brightness temperature is much lower than the Fe XII formation temperature, the radio and EUV enhancements are likely both related to the presence of concentrated magnetic flux, but do not arise from the same physical layer.


Key words: Sun: radio radiation -- Sun: UV radiation -- Sun: chromosphere -- Sun: transition region -- Sun: corona

Offprint request: T. Moran, tmoran@cspsw4.nascom.nasa.gov




© ESO 2001