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| Paper: |
First Image of the Corona of a Main-Sequence Star |
| Volume: |
154, Cool Stars, Stellar Systems and the Sun: Tenth Cambridge Workshop |
| Page: |
1942 |
| Authors: |
Benz, Arnold O.; Gudel, Manuel; Conway, John |
| Abstract: |
The binary system UV Cet A and B has been observed with the VLBA/VLA at 3.6 cm wavelength. Both dMe stars have been detected. The stronger, steady radio emitter of the two, UV Cet B, is resolved into at least two spatial components. Their relative intensities change during the 6.3 hours of observing time. One of the components is relatively stable and resolved, the other is possibly unresolved. The resolved component has a half-power diameter of about the size of the stellar photosphere or 2 x 1010 cm. The separation of the two components of UV Cet B is 4.4 (+/-0.4) x 1010 cm or 4-5 stellar radii. The alignment of the two components is along the axis of the binary orbit and thus probably close to the stellar rotation axis. The apparent trapping of the gyrosynchrotron emitting energetic electrons requires large coronal loops extending to several stellar radii. At the more variable source a magnetic field between 20 and 130 G is derived. |
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