Possible magnetic field variability during the 6.7 GHz methanol maser flares of G09.62+0.20

Details Possible magnetic field variability during the 6.7 GHz methanol maser flares of G09.62+0.20 Possible magnetic field variability during the 6.7 GHz methanol maser flares of G09.62+0.20

2009-04-30

arxiv.org/abs/0904.4806v1

Astronomy and Astrophysics

Astrophysics

Galaxy Astrophysics

4 pages, 3 figures, accepted for publication Astronomy and Astrophysics

Scientific paper

(Abridged) Recently, the magnetic field induced Zeeman splitting was measured for the strongest known 6.7 GHz methanol maser, which arises in the massive star forming region G09.62+0.20. This maser is one of a handful of periodically flaring methanol masers. The 100-m Effelsberg telescope was used to monitor the 6.7 GHz methanol masers of G09.62+0.20. With the exception of a two week period during the peak of the maser flare, we measure a constant magnetic field of B_||~11+-2 mG in the two strongest maser components of G09.62+0.20 that are separated by over 200 AU. In the two week period that coincides exactly with the peak of the maser flare of the strongest maser feature, we measure a sharp decrease and possible reversal of the Zeeman splitting. The exact cause of both maser and polarization variability is still unclear, but it could be related to either background amplification of polarized emission or the presence of a massive protostar with a close-by companion. Alternatively, the polarization variability could be caused by non-Zeeman effects related to the radiative transfer of polarized maser emission.

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