Large‐Angle Spectrometric Coronagraph Measurements of the Energetics of Coronal Mass Ejections

Vourlidas, A.; Subramanian, Prasad; Dere, K. P.; Howard, R. A.

doi:10.1086/308747

Cited by 260 publications

(275 citation statements)

References 30 publications

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“…Hence the parameters derived from the plasma emission model of the prominence/type IV burst of 1990 September 14 are comparable to Hα analyses of large erupting prominences. They are also comparable to values reported for CMEs by the coronagraphs aboard Skylab (Rust et al 1980), Solwind (Webb et al 1996), SMM (Hundhausen et al 1994) and SoHO (Lyons et al 1999;Vourlidas et al 2000), but are an order of magnitude above estimates from X-ray analyses (Hudson et al 1996;Gopalswamy et al 1997). The kinetic energy is near the upper limits of CME values.…”

Section: Estimate Of the Mass And Energetics Of The Ejected Plasma Blsupporting

confidence: 85%

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: Estimate Of the Mass And Energetics Of The Ejected Plasma Blsupporting

confidence: 85%

The dynamics of an erupting prominence

Klein¹,

Mouradian²

2002

A&A

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show abstract

“…However, a CME is a three dimensional structure with a significant depth along the line-of-sight. It has been reported earlier that such an assumption leads to underestimation of the CME mass by 15% (Vourlidas et al, 2000). We made several independent mass measurements for this event and found that the values are within 20% of the measured ones.…”

Section: Momentum Energy Exchange and Nature Of The Collisionsupporting

confidence: 68%

“…Assuming that the CME observed in white-light is due to Thomson scattered photospheric light from the electrons in the CME (Minnaert, 1930;Billings, 1966;Howard and Tappin, 2009), the recorded scattered intensity can then be converted into the number of electrons, and hence the mass of a CME can be estimated, assuming a completely ionized corona with a composition of 90% hydrogen and 10% helium. In earlier studies (Munro et al, 1979;Poland et al, 1981;Vourlidas et al, 2000), the mass of a CME was calculated assuming the CME location in the observer's plane of sky. We use the method of Colaninno and Vourlidas (2009) which is based on the Thomson scattering theory, to estimate the true propagation direction and true mass of both CMEs.…”

Section: Momentum Energy Exchange and Nature Of The Collisionmentioning

confidence: 99%

Interplanetary and Geomagnetic Consequences of Interacting CMEs of 13 – 14 June 2012

2018

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We report on the kinematics of two interacting CMEs observed on 13 and 14 June 2012. Both CMEs originated from the same active region NOAA 11504. After their launches which were separated by several hours, they were observed to interact at a distance of 100 R from the Sun. The interaction led to a moderate geomagnetic storm at the Earth with D st index of approximately, -86 nT. The kinematics of the two CMEs is estimated using data from the Sun Earth Connection Coronal and Heliospheric Investigation (SECCHI) onboard the Solar Terrestrial Relations Observatory (STEREO). Assuming a head-on collision scenario, we find that the collision is inelastic in nature. Further, the signatures of their interaction are examined using the in situ observations obtained by Wind and the Advance Composition Explorer (ACE) spacecraft. It is also found that this interaction event led to the strongest sudden storm commencement (SSC) (≈ 150 nT) of the present Solar Cycle 24. The SSC was of long duration, approximately 20 hours. The role of interacting CMEs in enhancing the geoeffectiveness is examined.

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“…The CME in particular contains a great deal of kinetic energy (e.g., Vourlidas et al 2000;Emslie et al 2005) show, for two major flares (the RHESSI flares of SOL2002-04-21T01:51 and SOL2002-07-23T00:35), that the CME kinetic energy is of the same order of magnitude as the radiated energy. In some well-studied cases (e.g., Robbrecht et al 2009) virtually no flare-like emissions can be detected at all.…”

Section: Large-scale Motions and A Mythmentioning

confidence: 99%

Global Properties of Solar Flares

2011

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This article broadly reviews our knowledge of solar flares. There is a particular focus on their global properties, as opposed to the microphysics such as that needed for magnetic reconnection or particle acceleration as such. Indeed solar flares will always remain in the domain of remote sensing, so we cannot observe the microscales directly and must understand the basic physics entirely via the global properties plus theoretical inference. The global observables include the general energetics-radiation in flares and mass loss in coronal mass ejections (CMEs)-and the formation of different kinds of ejection and global wave disturbance: the type II radio-burst exciter, the Moreton wave, the EIT "wave", and the "sunquake" acoustic waves in the solar interior. Flare radiation and CME kinetic energy can have comparable magnitudes, of order 10 32 erg each for an X-class event, with the bulk of the radiant energy in the visible-UV continuum. We argue that the impulsive phase of the flare dominates the energetics of all of these manifestations, and also point out that energy and momentum in this phase largely reside in the electromagnetic field, not in the observable plasma.

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Large‐Angle Spectrometric Coronagraph Measurements of the Energetics of Coronal Mass Ejections

Cited by 260 publications

References 30 publications

The dynamics of an erupting prominence

The dynamics of an erupting prominence

Interplanetary and Geomagnetic Consequences of Interacting CMEs of 13 – 14 June 2012

Global Properties of Solar Flares

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