Investigation of the Chromosphere–Corona Interface with the Upgraded Very High Angular Resolution Ultraviolet Telescope (VAULT2.0)

Vourlidas, A.; Beltran, Samuel Tun; Chintzoglou, Georgios; Eisenhower, Kevin; Korendyke, C. M.; Feldman, Ronen; Moser, John W.; Shea, J.; Johnson-Rambert, Mary; McMullin, D. R.; Stenborg, Guillermo; Shepler, Ed; Roberts, David E.

doi:10.1142/s2251171716400031

Cited by 11 publications

(10 citation statements)

References 28 publications

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“…This line is the most intensive line in the solar ultraviolet waveband (Curdt et al 2001), due to the large abundance of hydrogen in the solar atmosphere. Since the first rocket flight observations of the Sun with the Lyα line (Gabriel 1971;Samain et al 1975), there has been a number of space instruments for spectroscopic and imaging observations of the Sun in recent years (Wilhelm et al 1995;Kano et al 2012;Kobayashi et al 2012;Woods et al 2012;Vourlidas et al 2016).…”

Section: Introductionmentioning

confidence: 99%

The Response of the Lyα Line in Different Flare Heating Models

Hong

Liu

Ding

et al. 2019

ApJ

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The solar Lyα line is the strongest line in the ultraviolet waveband, and is greatly enhanced during solar flares. Here we present radiative hydrodynamic simulations of solar flares under different heating models, and calculate the response of this line taking into account non-equilibrium ionization of hydrogen and partial frequency redistribution. We find that in non-thermal heating models, the Lyα line can show a red or blue asymmetry corresponding to the chromospheric evaporation or condensation, respectively. The asymmetry may change from red to blue if the electron beam flux is large enough to produce a significant chromospheric condensation region. In the Lyα intensity lightcurve, there appears a dip when the change of asymmetry occurs. In thermal models, the Lyα line intensity peaks quickly and then falls, and the profile has an overall red asymmetry, which is similar to the profiles from heating by a soft electron beam. The Lyα profile shows a single red peak at the end of thermal heating, and the whole line is formed in a very small height range.

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Section: Introductionmentioning

confidence: 99%

The Response of the Lyα Line in Different Flare Heating Models

Hong

Liu

Ding

et al. 2019

ApJ

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“…In this work we present evidence for the "preventative" role magnetic topology can play for an erupting MFR and explain how it can 'kill' the eruption at its initial stage by destroying the rising magnetic structure. The event was captured by a unique and comprehensive set of instruments during the observing campaign in support of the launch of VAULT2.0 (Vourlidas et al 2016) on September 30, 2014.…”

Section: Introductionmentioning

confidence: 99%

Magnetic Flux Rope Shredding By a Hyperbolic Flux Tube: The Detrimental Effects of Magnetic Topology on Solar Eruptions

Chintzoglou

Vourlidas

Savcheva

et al. 2017

ApJ

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We present the analysis of an unusual failed eruption captured in high cadence and in many wavelengths during the observing campaign in support of the VAULT2.0 sounding rocket launch. The refurbished Very high Angular resolution Ultraviolet Telescope (VAULT2.0 ) is a Lyα (λ 1216Å) spectroheliograph launched on September 30, 2014. The campaign targeted active region NOAA AR 12172 and was closely coordinated with the Hinode and IRIS missions and several ground-based observatories (NSO/IBIS, SOLIS, and BBSO). A filament eruption accompanied by a low level flaring event (at the GOES C-class level) occurred around the VAULT2.0 launch. No Coronal Mass Ejection (CME) was observed. The eruption and its source region, however, were recorded by the campaign instruments in many atmospheric heights ranging from the photosphere to the corona in high cadence and spatial resolution. This is a rare occasion which enables -2 -us to perform a comprehensive investigation on a failed eruption. We find that a rising Magnetic Flux Rope-like (MFR) structure was destroyed during its interaction with the ambient magnetic field creating downflows of cool plasma and diffuse hot coronal structures reminiscent of "cusps". We employ magnetofrictional simulations to show that the magnetic topology of the ambient field is responsible for the destruction of the MFR. Our unique observations suggest that the magnetic topology of the corona is a key ingredient for a successful eruption.

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“…The HRI instruments will study the small-scale structures and highly dynamic events in the upper solar atmosphere. Lyα is the most intense emission line in the solar spectrum and affects planetary atmospheres, so it is of great interest; however, so far observations in Lyα are rare and were carried out mainly aboard sounding rockets (Korendyke et al 2001;Vourlidas et al 2010Vourlidas et al , 2016Chua et al 2013;Chintzoglou et al 2018) and the Transition Region and Coronal Explorer space observatory (Golub et al 1999). Table 6 shows the closest corresponding SPICE emission line to the EUI passband.…”

Section: The Euimentioning

confidence: 99%

Stereoscopic Measurements of Coronal Doppler Velocities

Podladchikova,

Harra,

Barczynski

et al. 2021

Preprint

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Context. The Solar Orbiter mission, with an orbit outside the Sun-Earth line and leaving the ecliptic plane, opens up opportunities for the combined analysis of measurements obtained by solar imagers and spectrometers. For the first time, different space spectrometers will be located at wide angles to each other, allowing three-dimensional (3D) spectroscopy of the solar atmosphere. Aims. The aim of this work is to prepare the methodology to facilitate the reconstruction of 3D vector velocities from two stereoscopic LOS Doppler velocity measurements using the Spectral Imaging of the Coronal Environment (SPICE) on board the Solar Orbiter and the near-Earth spectrometers, while widely separated in space. Methods. We develop the methodology using the libraries designed earlier for the STEREO mission but applied to spectroscopic data from the Hinode mission and the Solar Dynamics Observatory. We use well-known methods of static and dynamic solar rotation stereoscopy and the methods of EUV stereoscopic triangulation for optically-thin coronal EUV plasma emissions. We develop new algorithms using analytical geometry in space to determine the 3D velocity in coronal loops. Results. We demonstrate our approach with the reconstruction of 3D velocity vectors in plasma flows along "open" and "closed" magnetic loops. This technique will be applied to an actual situation of two spacecraft at different separations with spectrometers on board (SPICE versus the Interface Region Imaging Spectrograph (IRIS) and Hinode imaging spectrometer) during the Solar Orbiter nominal phase. We summarise how these observations can be coordinated.

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Investigation of the Chromosphere–Corona Interface with the Upgraded Very High Angular Resolution Ultraviolet Telescope (VAULT2.0)

Cited by 11 publications

References 28 publications

The Response of the Lyα Line in Different Flare Heating Models

The Response of the Lyα Line in Different Flare Heating Models

Magnetic Flux Rope Shredding By a Hyperbolic Flux Tube: The Detrimental Effects of Magnetic Topology on Solar Eruptions

Stereoscopic Measurements of Coronal Doppler Velocities

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