High sensitivity dynamic spectral search for flare star radio

Details High sensitivity dynamic spectral search for flare star radio High sensitivity dynamic spectral search for flare star radio

Aug 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...288..219a&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 288, no. 1, p. 219-230

Astronomy and Astrophysics

Astronomy

18

Flare Stars, Flux Density, Radio Astronomy, Radio Bursts, Radio Observation, Radio Spectra, Stellar Flares, Brightness Temperature, Circular Polarization, Cyclotron Radiation, Fine Structure, Plasma Radiation, Radio Telescopes, Sensitivity, Spectrum Analysis, Ultrahigh Frequencies

Scientific paper

We observed ten well-known flare stars with the Arcibo radio telescope at 1.4 GHz and 5 GHz, using a special observing technique to discriminate between real flares and radio freqeuncy interference. With a high sensitivity of 5.5 K/Jy at 1.4 GHz when averaged over a 50 MHz band, we are able to recognize flux enhancements as weak as approximately 6 mJy above the sky background variations. In about 85 hours of observation, about a dozen bursts were detected, only from AD Leo. All had flux densities lower than 70 mJy, which probably explains their lack of fine structures (except for the strongest one), such as were reported in the literature for stronger flares. Half of the bursts that we recorded are 100% circularly polarized, and half are not circularly polarized. Our results are a first attempt of reliable statistics on dMe flare rates at 1.4 GHz. The high brightness temperatures we infer for the observed bursts are interpreted in terms of coherent emission processes, either the cyclotron maser instability or plasma radiation. Efficiencies are comparable to those of solar or planetary radio emissions in the case of the cyclotron maser, and higher than the solar efficiency in the case of plasma radiation, with the caveat that there are great uncertainties in the coronal model and the source size.

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