The Ultraviolet Coronagraph Spectrometer for the solar and heliospheric observatory

Kohl, J. L.; Esser, Ruth; Gardner, L. D.; Habbal, Shadia Rifai; Daigneau, Peter; Dennis, E.; Nystrom, G.; Panasyuk, A. V.; Raymond, J. C.; Smith, Peter L.; Strachan, L.; Ballegooijen, A. A. van; Noci, G.; Fineschi, Silvano; Romoli, M.; Ciaravella, A.; Modigliani, A.; Huber, M. C. E.; Antonucci, E.; Benna, C.; Giordano, S.; Tondello, G.; Nicolosi, P.; Naletto, G.; Pernechele, Claudio; Spadaro, D.; Poletto, G.; Livi, S.; Lühe, O. von der; Geiss, J.; Timothy, J. G.; Gloeckler, G.; Allegra, A.; Basile, Giuseppe; Brusa, R. W.; Wood, Brian E.; Siegmund, Oswald H. W.; Fowler, William K.; Fisher, Richard R.; Jhabvala, M.

doi:10.1007/bf00733433

Cited by 388 publications

(152 citation statements)

References 22 publications

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“…Gosling et al 1981). This conclusion has been supported by remote sensing of the slow wind, for example by interplanetary scintillation measurements from Voyager 2 (Woo and Martin 1997) and via SOHO Ultraviolet Coronal Spectrometer (UVCS; Kohl et al 1995) Doppler measurements combined with context images from the Large Angle and Spectrometric Coronagraph (LASCO; Brueckner 1995) coronagraphs (Habbal et al 1997). SPP will for the first time allow us to definitively test this inference.…”

Section: Wispr Science Objectives and Requirementsmentioning

confidence: 91%

The Wide-Field Imager for Solar Probe Plus (WISPR)

et al. 2015

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mission designed to orbit as close as 7 million km (9.86 solar radii) from Sun center. WISPR employs a 95 • radial by 58 • transverse field of view to image the fine-scale structure of the solar corona, derive the 3D structure of the large-scale corona, and determine whether a dust-free zone exists near the Sun. WISPR is the smallest heliospheric imager to date yet it comprises two nested wide-field telescopes with large-format (2 K × 2 K) APS CMOS detectors to optimize the performance for their respective fields of view and to minimize the risk of dust damage, which may be considerable close to the Sun. The WISPR electronics are very flexible allowing the collection of individual images at cadences up to 1 second at perihelion or the summing of multiple images to increase the signal-to-noise when the spacecraft is further from the Sun. The dependency of the Thomson scattering emission of the corona on the imaging geometry dictates that WISPR will be very sensitive to the emission from plasma close to the spacecraft in contrast to the situation for imaging from Earth orbit. WISPR will be the first 'local' imager providing a crucial link between the large-scale corona and the in-situ measurements.

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Section: Wispr Science Objectives and Requirementsmentioning

confidence: 91%

The Wide-Field Imager for Solar Probe Plus (WISPR)

et al. 2015

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“…Several EUV spectrometers have helped in characterizing the physical parameters of coronal waves and associated phenomena: CDS (Harrison et al, 1995) and UVCS (Kohl et al, 1995) aboard SOHO, and EIS (Culhane et al, 2007) aboard Hinode. In the radio regime, the bulk of the information about wave-associated metric type II bursts comes from various ground-based radiospectrographs and radioheliographs.…”

Section: Observational Signaturesmentioning

confidence: 99%

Large-scale Globally Propagating Coronal Waves

Warmuth

2015

Living Rev. Sol. Phys.

156

140

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Large-scale, globally propagating wave-like disturbances have been observed in the solar chromosphere and by inference in the corona since the 1960s. However, detailed analysis of these phenomena has only been conducted since the late 1990s. This was prompted by the availability of high-cadence coronal imaging data from numerous spaced-based instruments, which routinely show spectacular globally propagating bright fronts. Coronal waves, as these perturbations are usually referred to, have now been observed in a wide range of spectral channels, yielding a wealth of information. Many findings have supported the "classical" interpretation of the disturbances: fast-mode MHD waves or shocks that are propagating in the solar corona. However, observations that seemed inconsistent with this picture have stimulated the development of alternative models in which "pseudo waves" are generated by magnetic reconfiguration in the framework of an expanding coronal mass ejection. This has resulted in a vigorous debate on the physical nature of these disturbances. This review focuses on demonstrating how the numerous observational findings of the last one and a half decades can be used to constrain our models of large-scale coronal waves, and how a coherent physical understanding of these disturbances is finally emerging. Article RevisionsLiving Reviews supports two ways of keeping its articles up-to-date:Fast-track revision. A fast-track revision provides the author with the opportunity to add short notices of current research results, trends and developments, or important publications to the article. A fast-track revision is refereed by the responsible subject editor. If an article has undergone a fast-track revision, a summary of changes will be listed here.Major update. A major update will include substantial changes and additions and is subject to full external refereeing. It is published with a new publication number.For detailed documentation of an article's evolution, please refer to the history document of the article's online version at http://dx

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“…Using data from Yohkoh and SOHO, Švestka (1996), Švestka et al (1998), Hudson (1999), andMcKenzie (2000) studied behaviors of regions above the top of the flare loop system, and displayed typical characteristics of the reconnection region and revealed important information above the reconnection process. Ciaravella et al (2002) analyzed spectral data obtained from the Ultraviolet Coronagraph Spectrometer (UVCS; Kohl et al 1995) on SOHO for an eruption on 1998 March 23. This event developed a slow CME propagating at speed of 100 km s −1 when the CME core was at the heliocentrical distance (namely the distance measured from the center of the Sun) of 3.5 R , and it reached a speed of 180 km s −1 as the core was at 15 R .…”

Section: Identifications Of the Current Sheet In The Solar Eruptive Ementioning

confidence: 99%

Review on Current Sheets in CME Development: Theories and Observations

et al. 2015

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We introduce how the catastrophe model for solar eruptions predicted the formation and development of the long current sheet (CS) and how the observations were used to recognize the CS at the place where the CS is presumably located. Then, we discuss the direct measurement of the CS region thickness by studying the brightness distribution of the CS region at different wavelengths. The thickness ranges from 10 4 km to about 10 5 km at heights between 0.27 and 1.16 R from the solar surface. But the traditional theory indicates that the CS is as thin as the proton Larmor radius, which is of order tens of meters in the corona. We look into the huge difference in the thickness between observations and theoretical expectations. The possible impacts that affect measurements and results are studied, and physical causes leading to a thick CS region in which reconnection can still occur at a reasonably fast rate are analyzed. Studies in both theories and observations suggest that the difference between the true value and the apparent value of the CS thickness is not significant as long as the CS could be recognised in observations. We review observations that show complex structures and flows inside the CS region and present recent numerical modelling results on some aspects of these structures. Both observations and numerical experiments indicate that the downward reconnection outflows are usually slower than the upward ones in the same eruptive event. Numerical simulations show that the complex structure inside CS and its temporal behavior as a result of turbulence and the Petschek-type slow-mode shock could probably account for the thick CS and fast reconnection. But whether the CS itself is that thick still remains unknown since, for the time being, we cannot measure the electric current directly in that region. We also review the most recent laboratory experiments of reconnection driven by energetic laser beams, and discuss some important topics for future works.

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The Ultraviolet Coronagraph Spectrometer for the solar and heliospheric observatory

Cited by 388 publications

References 22 publications

The Wide-Field Imager for Solar Probe Plus (WISPR)

The Wide-Field Imager for Solar Probe Plus (WISPR)

Large-scale Globally Propagating Coronal Waves

Review on Current Sheets in CME Development: Theories and Observations

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