Evidence for Chromospheric Evaporation in the Late Gradual Flare Phase from [ITAL]SOHO[/ITAL]/CDS Observations

Czaykowska, A.; Pontieu, Bart De; Alexander, David; Rank, G.

doi:10.1086/312176

Cited by 139 publications

(123 citation statements)

References 15 publications

(15 reference statements)

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“…Following work on eruptive events on the disk (cf. McAllister et al 1992;Hanaoka et al1994;van Driel-Gesztelyi et al 1997;Khan et al 1998;Czaykowska et al 1999), we identify these arches with the flare loops that form below the ejected structure and connect the flare ribbons which are expected to lie behind the limb in the present event. At the end of our Hα observations the loop tops were at a height of 45 000 km and still slowly rising.…”

Section: Hα Observationsmentioning

confidence: 53%

The dynamics of an erupting prominence

Klein¹,

Mouradian²

2002

A&A

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Abstract. Hα full disk observations and radio interferometry at decimetre and metre wavelengths are used to probe the dynamics of ejecta and electron acceleration during a solar eruptive event on 1990 September 14. An erupting prominence and a moving type IV radio source are shown to trace a common magnetic structure during its rise from ∼10 Mm to 3 R above the limb. The height-time plot excludes a purely ballistic flight in the height range (0.5-3) R , but is consistent with both constant acceleration and constant velocity at heights ≥0.5 R . A plasma model of the radio emission is used to infer the mass and energetics of the ejected material. Electrons are accelerated in the surroundings of the rising structure, and in two flares up to 70 • away from the prominence. Radio observations provide evidence for large-scale interconnecting loops, but a physical connection between the eruption and the remote flares cannot be demonstrated.

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Section: Hα Observationsmentioning

confidence: 53%

The dynamics of an erupting prominence

Klein¹,

Mouradian²

2002

A&A

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“…Magnetogram sequences for the day also show motions of the magnetic flux at the microflares' site. Czaykowska et al (1999) also reported downflows of ∼+60 km s −1 into a sunspot during an M-class flare observed by CDS with no obvious origin of such flows. As a possible cause for the strong downflows into the penumbra associated with our microflares we propose solar gravitation.…”

Section: Discussionmentioning

confidence: 86%

“…Of special importance in this context are observations where the slit is situated directly at the flare energy deposit site. In one of the first CDS flare studies, Czaykowska et al (1999) find downflows at the end of bright post flare loops but also strong, hot upflows at their outer edge even in the late phase of an M class flare. Brosius (2003) also finds upflows in the impulsive phase and "warm rain" due to cooling flare plasma in an important flare.…”

Section: Introductionmentioning

confidence: 99%

Multi-wavelength fine structure and mass flows in solar microflares

Berkebile-Stoiser¹,

Gömöry

Veronig³

et al. 2009

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“…Various observations of largescale two-ribbon flares have been carried out. For example, Czaykowska et al (1999) and Del Zanna et al (2006b) reported SOHO/CDS observations of arcade of hot loops during the gradual phase of two large flares (the second was the X17 flare of 2003 October 28). Both papers reported strong blue-shifts in hot Fe xvi (3 MK) and Fe xix (9 MK) lines located at the outer edges of the flare ribbons.…”

Section: Introductionmentioning

confidence: 99%

The 22 May 2007 B-class flare: new insights fromHinodeobservations

Zanna¹,

Mitra-Kraev²,

Bradshaw

et al. 2010

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We present multi-wavelength observations of a small B-class flare which occurred on the Sun on 2007 May 22. The observations include data from Hinode, GOES, TRACE and the Nobeyama Radioheliograph. We obtained spatially and spectrally-resolved information from the Hinode EUV Imaging Spectrometer (EIS) during this event. The temporal and temperature coverage of the EIS observations provides new insights into our understanding of chromospheric evaporation and cooling. The flare showed many "typical" features, such as brightenings in the ribbons, hot (10 MK) loop emission and subsequent cooling. We also observed a new feature, strong (up to 170 km s −1 ) blue-shifted emission in lines formed around 2-3 MK, located at the footpoints of the 10 MK coronal emission and within the ribbons. Electron densities at 2 MK in the kernels are high, of the order of 10 11 cm −3 , suggesting a very narrow layer where the chromospheric evaporation occurs. We have run a non-equilibrium hydrodynamic numerical simulation using the HYDRAD code to study the cooling of the 10 MK plasma, finding good agreement between the predicted and observed temperatures, densities and ion populations. Line blending for some potentially useful diagnostic lines for flares, which are observed with Hinode/EIS, is also discussed.

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Evidence for Chromospheric Evaporation in the Late Gradual Flare Phase from [ITAL]SOHO[/ITAL]/CDS Observations

Cited by 139 publications

References 15 publications

The dynamics of an erupting prominence

The dynamics of an erupting prominence

Multi-wavelength fine structure and mass flows in solar microflares

The 22 May 2007 B-class flare: new insights fromHinodeobservations

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