Observation of the powerful solar flare of October 27, 2002 on the far side of the sun

V. I. Vybornov; M. A. Livshits; L. K. Kashapova; I. G. Mitrofanov; D. V. Golovin; A. S. Kozyrev; M. L. Litvak; A. B. Sanin; V. I. Tret'yakov; W. Boynton; K. Shinohara; D. Hamara

doi:10.1134/S1063772912100083

Observation of the powerful solar flare of October 27, 2002 on the far side of the sun

V. I. Vybornov, M. A. Livshits, L. K. Kashapova, I. G. Mitrofanov, D. V. Golovin, A. S. Kozyrev, M. L. Litvak, A. B. Sanin, V. I. Tret'yakov, W. Boynton, K. Shinohara, D. Hamara

Lunar and Planetary Lab

Research output: Contribution to journal › Article › peer-review

5 Scopus citations

Abstract

Observations of the hard X-ray and radio event of October 27, 2002 are analyzed. This flare was observed from near-Martian orbit by the HEND instrument developed at the Space Research Institute of the Russian Academy of Sciences and installed on the Mars Odyssey satellite. Although this powerful flare was observed far over the eastern solar limb, the extended source associated with the flare was detected by RHESSI at energies up to about 60 keV. The eruptive event was observed in the radio at the Nobeyama Radio Observatory. The properties of the X-ray radiation are used to calculate the spectrum of the accelerated electrons responsible for the observed radiation, assuming that the target is thick for a Martian observer and thin for a terrestrial observer. The results are compared with the results of radio observations. The conditions for electron propagation in the corona are discussed.

Original language	English (US)
Pages (from-to)	805-812
Number of pages	8
Journal	Astronomy Reports
Volume	56
Issue number	10
DOIs	https://doi.org/10.1134/S1063772912100083
State	Published - Oct 2012

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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@article{6da792c72158466580ea5d0eb5fa2eb0,

title = "Observation of the powerful solar flare of October 27, 2002 on the far side of the sun",

abstract = "Observations of the hard X-ray and radio event of October 27, 2002 are analyzed. This flare was observed from near-Martian orbit by the HEND instrument developed at the Space Research Institute of the Russian Academy of Sciences and installed on the Mars Odyssey satellite. Although this powerful flare was observed far over the eastern solar limb, the extended source associated with the flare was detected by RHESSI at energies up to about 60 keV. The eruptive event was observed in the radio at the Nobeyama Radio Observatory. The properties of the X-ray radiation are used to calculate the spectrum of the accelerated electrons responsible for the observed radiation, assuming that the target is thick for a Martian observer and thin for a terrestrial observer. The results are compared with the results of radio observations. The conditions for electron propagation in the corona are discussed.",

author = "Vybornov, {V. I.} and Livshits, {M. A.} and Kashapova, {L. K.} and Mitrofanov, {I. G.} and Golovin, {D. V.} and Kozyrev, {A. S.} and Litvak, {M. L.} and Sanin, {A. B.} and Tret'yakov, {V. I.} and W. Boynton and K. Shinohara and D. Hamara",

note = "Funding Information: We thank the RHESSI and SOHO teams and the Nobeyama Radio Observatory and RSTN for providing free access to their data. SOHO is a cooperative project of the European Space Agency and NASA. This work was supported by the Russian Foundation for Basic Research (project 11-02-00264) and the Ministry of Education and Science of the Russian Federation.",

year = "2012",

month = oct,

doi = "10.1134/S1063772912100083",

language = "English (US)",

volume = "56",

pages = "805--812",

journal = "Astronomy Reports",

issn = "1063-7729",

publisher = "Pleiades Publishing",

number = "10",

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TY - JOUR

T1 - Observation of the powerful solar flare of October 27, 2002 on the far side of the sun

AU - Vybornov, V. I.

AU - Livshits, M. A.

AU - Kashapova, L. K.

AU - Mitrofanov, I. G.

AU - Golovin, D. V.

AU - Kozyrev, A. S.

AU - Litvak, M. L.

AU - Sanin, A. B.

AU - Tret'yakov, V. I.

AU - Boynton, W.

AU - Shinohara, K.

AU - Hamara, D.

N1 - Funding Information: We thank the RHESSI and SOHO teams and the Nobeyama Radio Observatory and RSTN for providing free access to their data. SOHO is a cooperative project of the European Space Agency and NASA. This work was supported by the Russian Foundation for Basic Research (project 11-02-00264) and the Ministry of Education and Science of the Russian Federation.

PY - 2012/10

Y1 - 2012/10

N2 - Observations of the hard X-ray and radio event of October 27, 2002 are analyzed. This flare was observed from near-Martian orbit by the HEND instrument developed at the Space Research Institute of the Russian Academy of Sciences and installed on the Mars Odyssey satellite. Although this powerful flare was observed far over the eastern solar limb, the extended source associated with the flare was detected by RHESSI at energies up to about 60 keV. The eruptive event was observed in the radio at the Nobeyama Radio Observatory. The properties of the X-ray radiation are used to calculate the spectrum of the accelerated electrons responsible for the observed radiation, assuming that the target is thick for a Martian observer and thin for a terrestrial observer. The results are compared with the results of radio observations. The conditions for electron propagation in the corona are discussed.

AB - Observations of the hard X-ray and radio event of October 27, 2002 are analyzed. This flare was observed from near-Martian orbit by the HEND instrument developed at the Space Research Institute of the Russian Academy of Sciences and installed on the Mars Odyssey satellite. Although this powerful flare was observed far over the eastern solar limb, the extended source associated with the flare was detected by RHESSI at energies up to about 60 keV. The eruptive event was observed in the radio at the Nobeyama Radio Observatory. The properties of the X-ray radiation are used to calculate the spectrum of the accelerated electrons responsible for the observed radiation, assuming that the target is thick for a Martian observer and thin for a terrestrial observer. The results are compared with the results of radio observations. The conditions for electron propagation in the corona are discussed.

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Observation of the powerful solar flare of October 27, 2002 on the far side of the sun

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