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Warmuth, A.; Hanslmeier, A.; Messerotti, M.; Cacciani, A.; Moretti, P. F.; Otruba, W.

doi:10.1023/a:1005284918367

Cited by 27 publications

(30 citation statements)

References 10 publications

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“…The same scales are those obtained by the analysis of the background locations maintaining spatial resolution (Moretti et al 2001a). Recently, observations in Hα and NaI D lines have shown a simultaneous occurrence of the impulsive brightenings (Warmuth et al 2000;Moretti et al 2001b). For this reason we suggest the impulsive brightenings are related to the explosive events in the upper atmosphere.…”

Section: The Observationssupporting

confidence: 64%

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An interpretation of the $\vec{I-V}$ phase background based on observed plasma jets

Moretti

Cacciani²,

Hanslmeier

et al. 2002

A&A

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Abstract. The presence of a solar background in the phase difference between the intensity and velocity (I − V) p-mode oscillation signals recently has been interpreted in terms of downflows due to convection (Skartlien & Rast 2000) or due to chromospheric explosive events (Moretti et al. 2001a). In support of the latter, we present I and V characteristics of impulsive brightenings observed in the NaI D lines, show that these reproduce the frequency dependence of the I − V modulation background, and show that explanations invoking more frequently occurring phenomena such as seismic events are not likely in low-l modulation data.

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Section: The Observationssupporting

confidence: 64%

“…Many impulsive brightenings in the NaI D lines have been detected at the Solar Kanzelhöhe Observatory (Warmuth et al 2000;Moretti et al 2001b).…”

Section: The Observationsmentioning

confidence: 98%

An interpretation of the $\vec{I-V}$ phase background based on observed plasma jets

Moretti

Cacciani²,

Hanslmeier

et al. 2002

A&A

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show abstract

“…This active region has been the subject of a number of studies owing to its unusually active nature for the period of the solar cycle during which it was observed. Warmuth et al (2000) describe the evolution of this region in white light and Hα data, which was dominated by a large, rapidly rotating delta spot. Sterling & Moore (2001) also studied this region in terms of its sigmoidal morphology and a series of homologous flares occurring on the 1st and 2nd May 1998, just prior to the appearance of a clear transequatorial connection between active regions.…”

Section: Discussionmentioning

confidence: 99%

The association of transequatorial loops in the solar corona with coronal mass ejection onset

Glover¹,

Harra²,

Matthews³

et al. 2003

A&A

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Abstract.It has been shown that transequatorial loops can disappear in association with the onset of a coronal mass ejection (CME) (Khan & Hudson 2000). We extend this result by considering a larger sample of transequatorial loop systems (TLS) to investigate their associated flaring and CME activity. We find 10 of a total 18 TLS considered here to be associated with flaring and CME onset originating from a connected active region. A total 33 cases of flaring and associated CME onset are observed from these 10 systems during their lifetime. We observe the influence of this activity on the TLS in each case. In contrast to the Khan & Hudson result, we find evidence that transequatorial loop eruption leading to soft X-ray brightening equivalent in temperature to a B-class flare is equally as common as dimming in the corona. Consequently we conclude that the scenario observed by Khan & Hudson is not universal and that other types of CME-TLS association occur. It was found that for transequatorial loops that were associated with CMEs the asymmetry in longitude was larger than for those that were not associated to a CME by 10 • . In addition, the extent in latitude (as a measure of the loop length) was nearly twice as large for those TLS associated with CMEs than those that were not. The asymmetry in latitude was actually on average larger for those TLS not associated with CMEs, than for those that were. This suggests that differential rotation is not a major contributor to the production of CMEs from transequatorial loops. Instead it is more likely for a CME to be produced if the loop is long, and if there is a large asymmetry in longitude. The implications of these results for CME onset prediction are discussed.

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“…A flare and coronal mass ejection (CME) began at 22:30 UT on 1998 May 1, soon after this magnetogram sequence ended at 21:29. This active region is of special interest because it produced a large number of flares and eruptive events during its transit across the solar disk, and has been the subject of many other studies Pohjolainen et al 2001;Wang et al 2002;Warmuth et al 2000;Xia et al 2002). In the same section, we also present a ''data movie'' we made of AR 8210's line-of-sight field on 1 May 1998, from MDI full-disk data.…”

Section: Why Investigate Photospheric Velocities?mentioning

confidence: 99%

ILCT: Recovering Photospheric Velocities from Magnetograms by Combining the Induction Equation with Local Correlation Tracking

Welsch

Fisher

Abbett

et al. 2004

ApJ

189

199

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Untitled

Cited by 27 publications

References 10 publications

An interpretation of the $\vec{I-V}$ phase background based on observed plasma jets

An interpretation of the $\vec{I-V}$ phase background based on observed plasma jets

The association of transequatorial loops in the solar corona with coronal mass ejection onset

ILCT: Recovering Photospheric Velocities from Magnetograms by Combining the Induction Equation with Local Correlation Tracking

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