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Borovik, Aleksandr; Myachin, D. Yu.

doi:10.1023/a:1013859722017

Cited by 11 publications

(5 citation statements)

References 3 publications

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“…We are aware of a single paper describing a similar phenomenon (Borovik & Myachin 2002). Some parts of the ring structure resembled a quasi-stationary "EIT wave" stopping at the separatrix surface.…”

Section: Outline Of the Coronal Magnetic Configurationmentioning

confidence: 96%

“…The ring structure looked like a flare ribbon occulted by a multitude of dark absorbing features crossing it (see the western part of the ring structure in figures 4c-h and its southern part in figure 7g labeled "Stripe"). We are aware of a single paper describing a similar phenomenon (Borovik & Myachin 2002). Some parts of the ring structure resembled a quasistationary "EIT wave" stopping at the separatrix surface.…”

Section: Outline Of the Coronal Magnetic Configurationmentioning

confidence: 96%

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Eruptions of Magnetic Ropes in Two Homologous Solar Events of 2002 June 1 and 2: a Key to Understanding an Enigmatic Flare

Meshalkina¹,

Uralov²,

Grechnev³

et al. 2009

Publications of the Astronomical Society of Japan

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The goal of this paper is to understand the drivers, configurations, and scenarios of two similar eruptive events, which occurred in the same solar active region 9973 on 2002 June 1 and 2. The June 2 event was previously studied by Sui, Holman, and Dennis (2006, ApJ, 646, 605; 2008, Adv. Space Res., 41, 976), who concluded that it was challenging for popular flare models. Using multi-spectral data, we analyzed a combination of the two events. Each of the events exhibited an evolving cusp-like feature. We have revealed that these apparent "cusps" were most likely mimicked by twisted magnetic flux ropes, but unlikely to be related to the inverted Y-like magnetic configuration in the standard flare model. The ropes originated inside a funnel-like magnetic domain whose base was bounded by an EUV ring structure, and the top was associated with a coronal null point. The ropes appear to be the major drivers for the events, but their rise was not triggered by reconnection in the coronal null point. We propose a scenario and a three-dimensional scheme for these events in which the filament eruptions and flares were caused by interaction of the ropes.

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Section: Outline Of the Coronal Magnetic Configurationmentioning

confidence: 96%

Section: Outline Of the Coronal Magnetic Configurationmentioning

confidence: 96%

Eruptions of Magnetic Ropes in Two Homologous Solar Events of 2002 June 1 and 2: a Key to Understanding an Enigmatic Flare

Meshalkina¹,

Uralov²,

Grechnev³

et al. 2009

Publications of the Astronomical Society of Japan

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“…The study of low-power flares gained fresh momentum in works dealing with flares occurring far from sunspots in regions of the quiet chromosphere [Borovik, Myachin, 2002]. Previously unknown or extremely rare pre-flare activations were detected: type-S vortex structures, dark cells, ribbon channels.…”

Section: Study Of Solar Flaresmentioning

confidence: 99%

“…Spotless flares, like flares in active regions, were proved to appear and develop at the boundaries of cells of chromospheric and magnetic networks (see Figure 8). The magnetic field topology plays a decisive role in the development of flares [Borovik, Myachin, 2010;Borovik et al, 2014]. Flare nodes usually appear in the close vicinity of magnetic hills with a strength of 80 G and higher.…”

Section: Study Of Solar Flaresmentioning

confidence: 99%

Solar activity research at the Baikal Astrophysical Observatory of ISTP SB RAS

Borovik¹,

Головко²,

Golovko

et al. 2019

Solar-Terrestrial Physics

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The article presents the main results of solar studies carried out at the Baikal Astrophysical Observatory (BAO) of the Institute of Solar-Terrestrial Physics SB RAS (ISTP SB RAS) for 40 years. It outlines the history of BAO and lists its telescopes. Much attention is given to the Large Solar Vacuum Telescope (LSVT) designed to observe solar formations with high spatial and spectral resolution. Technical parameters of this instrument are specified along with some results of the studies carried out with it. Information about the full-disk chromospheric telescope and scientific problems solved with it is represented together with the basic scientific results. The telescope is used to study solar activity complexes and solar flares. References to the basic publications that have used BAO results are presented.

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“…In spite of the Sun, red dwarf stars are mostly known to have a different dynamo because of full convective outer atmosphere. However, in the last years, some studies showed that flares on the Sun do not have to be located upon the spotted areas on the Sun (Borovik et al 2007). In addition, it should be kept in mind that most of the studies have been done with using the data obtained from white-light flare observations, but a whitelight flare does not have to occur in a flare process.…”

Section: The Relation Between Stellar Spot and Flare Activitiesmentioning

confidence: 99%

Rotation Modulations and Distributions of the Flare Occurrence Rates on the Surface of Five UV Ceti Type Stars

Dal¹,

Evren²

2011

Publications of the Astronomical Society of Japan

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In this study, we discuss stellar spots, stellar flares and also the relation between these two magnetic proccess that take place on UV Ceti stars. In addition, the hypothesis about slow flares described by Gurzadian (1986) will be discussed. All these discussions are based on the results of three years of observations of the UV Ceti type stars AD Leo, EV Lac, V1005 Ori, EQ Peg and V1054 Oph. First of all, the results show that the stellar spot activity occurs on the stellar surface of EV Lac, V1005 Ori and EQ Peg, while AD Leo does not show any short-term variability and V1054 Oph does not exhibits any variability. We report new ephemerides, for EV Lac, V1005 Ori and EQ Peg, obtained from the time series analyses. The phases, computed in intervals of 0.10 phase length, where the mean flare occurence rates get maximum amplitude, and the phases of rotational modulation were compared to investigate whether there is any longitudinal relation between stellar flares and spots. Although, the results show that flare events are related with spotted areas on the stellar surfaces in some of the observing seasons, we did not find any clear correlation among them. Finally, it is tested whether slow flares are the fast flares occurring on the opposite side of the stars according to the direction of the observers as mentioned in the hypothesis developed by Gurzadian (1986). The flare occurence rates reveal that both slow and fast flares can occur in any rotational phases. The flare occurence rates of both fast and slow flares are varying in the same way along the longitudes for all program stars. These results are not expected based on the case mentioned in the hypothesis.

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Cited by 11 publications

References 3 publications

Eruptions of Magnetic Ropes in Two Homologous Solar Events of 2002 June 1 and 2: a Key to Understanding an Enigmatic Flare

Eruptions of Magnetic Ropes in Two Homologous Solar Events of 2002 June 1 and 2: a Key to Understanding an Enigmatic Flare

Solar activity research at the Baikal Astrophysical Observatory of ISTP SB RAS

Rotation Modulations and Distributions of the Flare Occurrence Rates on the Surface of Five UV Ceti Type Stars

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