Radio Emission from Flare Star V371 Orionis

Patston, G.E.; Slee, O. B.; Solomon, L. H.

doi:10.1038/199991a0

Cited by 36 publications

(10 citation statements)

References 1 publication

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“…The flux densities recorded for these flares at cm wavelengths are typically in millijanskys, and the highest recorded was only a fraction of a Jy. However, at lower frequencies, particularly at decameter wavelengths, flux densities of some of the flares recorded are ∼100 Jy (Abdul-Aziz et al 1995) to ∼ 10 4 Jy (Slee 1963). The highest luminosity of any flare star(s) in the metre wave band is ∼230 Jy at 136 MHz as recorded by Slee & Higgins (1969) towards the Orion nebula located ∼400 pc away.…”

Section: Distance To the Gcrt And Its Classificationmentioning

confidence: 99%

Circularly Polarized Emission From the Transient Bursting Radio Source GCRT J1745 – 3009

Roy

Hyman

Pal

et al. 2010

ApJ

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We report detection of strong circularly polarized emission from the transient bursting source GCRT J1745-3009 based on new analysis of 325 MHz GMRT observations conducted on 28 September 2003. We place 8 R ⊙ as the upper limit on the size of the emission region. The implied high brightness temperature required for an object beyond 1 pc and the high fraction of circular polarization firmly establish the emission as coherent. Electron cyclotron or plasma emission from a highly subsolar magnetically dominated dwarf located ≤4 kpc away could have given rise to the GCRT radio emission.

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Section: Distance To the Gcrt And Its Classificationmentioning

confidence: 99%

Circularly Polarized Emission From the Transient Bursting Radio Source GCRT J1745 – 3009

Roy

Hyman

Pal

et al. 2010

ApJ

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“…Early radio observations targeted optically-active M dwarf stars and were carried out at meter wavelengths using single-dish radio telescopes (Lovell 1964(Lovell , 1969Higgins et al 1968;Slee 1963;Spangler et al 1974a;Spangler & Moffett 1976;Nelson et al 1979). These observations were sensitive to flares with intensities greater than several hundred millijanskys.…”

Section: Introductionmentioning

confidence: 99%

154 MHz Detection of Faint, Polarized Flares from UV Ceti

Lynch

Lenc

Kaplan

et al. 2017

ApJL

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We have detected four flares from UV Ceti at 154 MHz using the Murchison Widefield Array. The flares have flux densities between 10-65 mJy -a factor of 100 fainter than most flares in the literature at these frequencies -and are only detected in polarization. The circular polarized fractions are limited to > 27% at 3σ confidence and two of the flares exhibit polarity reversal. We suggest that these flares occur periodically on a time scale consistent with the rotational period of UV Ceti. During the brightest observed flare, we also detect significant linear polarization with polarization fraction > 18%. Averaging the data in 6-minute, 10 MHz frequency bins we find that the flux density of these flares does not vary over the 30 MHz bandwidth of the Murchison Widefield Array, however we cannot rule out finer time-frequency structure. Using the measured flux densities for the flares, we estimate brightness temperatures between (10 13 − 10 14 ) K, indicative of a coherent emission mechanism. The brightness temperature and polarization characteristics point to the electron cyclotron maser mechanism. We also calculate the flare rates given our four observed flares and compare them to flare rates for the set of M dwarf stars with known 100-200 MHz flares. Our measurement is the first for flares with intensities < 100 mJy at 100-200 MHz.

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“…Recently, the MWA has been successful in detecting faint, polarised flares from the well-known flare star UV Ceti (Lynch et al 2017), uncovering a population of lowfrequency flares two orders of magnitude fainter than single-dish detections made before the 1980s (e.g. Nelson et al 1979;Spangler, Shawhan, & Rankin 1974;Lovell 1964;Slee 1963).…”

Section: M-dwarf Flaresmentioning

confidence: 99%

A VOEvent-based automatic trigger system for the Murchison Widefield Array

Hancock

Anderson

Williams

et al. 2019

Publ. Astron. Soc. Aust.

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The Murchison Widefield Array (MWA) is an electronically steered low frequency (< 300 MHz) radio interferometer, with a 'slew' time less than 8 seconds. Low frequency (∼ 100 MHz) radio telescopes are ideally suited for rapid-response follow-up of transients due to their large field of view, the inverted spectrum of coherent emission, and the fact that the dispersion delay between a 1GHz and 100MHz pulse is on the order of 1 − 10 min for dispersion measures of 100 − 2000 pc/cm 3 . The MWA has previously been used to provide fast follow up for transient events including gamma-ray bursts, fast radio bursts, and gravitational waves, using systems that respond to gamma-ray coordinates network (GCN) packet-based notifications. We describe a system for automatically triggering MWA observations of such events, based on VOEvent triggers, which is more flexible, capable, and accurate than previous systems. The system can respond to external multi-messenger triggers, which makes it well-suited to searching for prompt coherent radio emission from gamma-ray bursts, the study of fast radio bursts and gravitational waves, single pulse studies of pulsars, and rapid follow-up of high-energy superflares from flare stars. The new triggering system has the capability to trigger observations in both the regular correlator mode (limited to ≥ 0.5 s integrations) or using the Voltage Capture System (VCS, 0.1 ms integration) of the MWA, and represents a new mode of operation for the MWA. The upgraded standard correlator triggering capability has been in use since MWA observing semester 2018B (July-Dec 2018), and the VCS and buffered mode triggers will become available for observing in a future semester.

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Radio Emission from Flare Star V371 Orionis

Cited by 36 publications

References 1 publication

Circularly Polarized Emission From the Transient Bursting Radio Source GCRT J1745 – 3009

Circularly Polarized Emission From the Transient Bursting Radio Source GCRT J1745 – 3009

154 MHz Detection of Faint, Polarized Flares from UV Ceti

A VOEvent-based automatic trigger system for the Murchison Widefield Array

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