The Ultraviolet Spectrometer and Polarimeter on the Solar Maximum Mission

Woodgate, B. E.; Tandberg-Hanssen, E.; Bruner, E. C.; Beckers, J. M.; Brandt, John C.; Henze, W.; Hyder, C. L.; Kalet, M. W.; Kenny, Patrick; Knox, E. D.; Michalitsianos, A. G.; Rehse, R.; Shine, R. A.; Tinsley, H. D.

doi:10.1007/bf00151385

Cited by 148 publications

(72 citation statements)

References 3 publications

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“…The visibility of prominences in the transition-region (TR) lines was previously demonstrated by Poland & Tandberg-Hanssen (1983) on UV observations of a prominence obtained on November 20, 1980 by the Ultraviolet Spectrometer and Polarimeter (Woodgate et al 1980) onboard the Solar Maximum Mission. For filaments, the TR O v line emission from PCTR was assumed in Schwartz et al (2004).…”

Section: Discussionmentioning

confidence: 79%

Non-LTE modelling of prominence fine structures using hydrogen Lyman-line profiles

Schwartz

Gunár

Curdt

2015

A&A

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Aims. We perform a detailed statistical analysis of the spectral Lyman-line observations of the quiescent prominence observed on May 18, 2005. Methods. We used a profile-to-profile comparison of the synthetic Lyman spectra obtained by 2D single-thread prominence finestructure model as a starting point for a full statistical analysis of the observed Lyman spectra. We employed 2D multi-thread finestructure models with random positions and line-of-sight velocities of each thread to obtain a statistically significant set of synthetic Lyman-line profiles. We used for the first time multi-thread models composed of non-identical threads and viewed at line-of-sight angles different from perpendicular to the magnetic field. Results. We investigated the plasma properties of the prominence observed with the SoHO/SUMER spectrograph on May 18, 2005 by comparing the histograms of three statistical parameters characterizing the properties of the synthetic and observed line profiles. In this way, the integrated intensity, Lyman decrement ratio, and the ratio of intensity at the central reversal to the average intensity of peaks provided insight into the column mass and the central temperature of the prominence fine structures.

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Section: Discussionmentioning

confidence: 79%

Non-LTE modelling of prominence fine structures using hydrogen Lyman-line profiles

Schwartz

Gunár

Curdt

2015

A&A

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“…The spectral ranges that IRIS observes have previously been studied at lower resolution using rockets (Bates et al, 1969;Fredga, 1969;Kohl and Parkinson, 1976;Allen and McAllister, 1978;Morrill and Korendyke, 2008;West et al, 2011;Dere, Bartoe, and Brueckner, 1984), balloons (Lemaire, 1969;Lemaire and Skumanich, 1973;Samain and Lemaire, 1985;Staath and Lemaire, 1995), or satellites (Doschek and Feldman, 1977;Bonnet et al, 1978;Woodgate et al, 1980;Roussel-Dupre and Shine, 1982; Billings, Roussel-Dupre, and Francis, 1977;Poland and Tandberg-Hanssen, 1983;Kingston et al, 1982). IRIS draws on heritage solar instrumentation, such as the Transition Region and Coronal Explorer (TRACE: Handy et al, 1999), the Helioseismic and Magnetic Imager (HMI: Scherrer et al, 2012) and the Atmospheric Imaging Assembly (AIA: Lemen et al, 2012) onboard the Solar Dynamics Observatory (SDO: Pesnell, Thompson, and Chamberlin, 2012), and it exploits advances in novel, high-throughput, and high-resolution instru- mentation, efficient numerical simulation codes, and powerful, massively parallel supercomputers to aid interpretation of the data.…”

Section: Introductionmentioning

confidence: 99%

The Interface Region Imaging Spectrograph (IRIS)

et al. 2014

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The Interface Region Imaging Spectrograph (IRIS) small explorer spacecraft provides simultaneous spectra and images of the photosphere, chromosphere, transition region, and corona with 0.33 -0.4 arcsec spatial resolution, two-second temporal resolution, and 1 km s −1 velocity resolution over a field-of-view of up to 175 arcsec × 175 arcsec. . IRIS is sensitive to emission from plasma at temperatures between 5000 K and 10 MK and will advance our understanding of the flow of mass and energy through an interface region, formed by the chromosphere and transition region, between the photosphere and corona. This highly structured and dynamic region not only acts as the conduit of all mass and energy feeding into the corona and solar wind, it also requires an order of magnitude more energy to heat than the corona and solar wind combined. The IRIS investigation includes a strong numerical modeling component based on advanced radiative-MHD codes to facilitate interpretation of observations of this complex region. Approximately eight Gbytes of data (after compression) are acquired by B. De Pontieu (B) ·Harvard-Smithsonian Astrophysical Observatory, 60 Garden Street, Cambridge, MA 02138, USA

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“…(1) Brekke (1993b), (2) Shine & Frank (2000), Woodgate et al (1980), (3) Curdt et al (2001), (4) http://solg2.bnsc.rl.ac.uk/atlas/atlas.shtml, (5) Brekke et al (2000), (6) Rottman et al (1993), (7) EUV Grating Spectrograph, Woods & Rottman (1990), (8) Leitherer et al (2001), Bohlin et al (2001).…”

Section: Introductionmentioning

confidence: 99%

HST/STIS high resolution echelle spectra ofαCentauri A (G2 V)

Pagano¹,

Linsky²,

Valenti³

et al. 2004

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Abstract. We describe and analyze HST/STIS observations of the G2 V star α Centauri A (α Cen A, HD 128620), a star similar to the Sun. The high resolution echelle spectra obtained with the E140H and E230H gratings cover the complete spectral range 1133−3150 Å with a resolution of 2.6 km s −1 , an absolute flux calibration accurate to ±5%, and an absolute wavelength accuracy of 0.6-1.3 km s −1 . We present here a study of the E140H spectrum covering the 1140-1670 Å spectral range, which includes 671 emission lines representing 37 different ions and the molecules CO and H 2 . For α Cen A and the quiet and active Sun, we intercompare the redshifts, nonthermal line widths, and parameters of two Gaussian representations of transition region lines (e.g., Si , C ), infer the electron density from the O  intersystem lines, and compare their differential emission measure distributions. One purpose of this study is to compare the α Cen A and solar UV spectra to determine how the atmosphere and heating processes in α Cen A differ from the Sun as a result of the small differences in gravity, age, and chemical composition of the two stars. A second purpose is to provide an excellent high resolution UV spectrum of a solar-like star that can serve as a proxy for the Sun observed as a point source when comparing other stars to the Sun.

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The Ultraviolet Spectrometer and Polarimeter on the Solar Maximum Mission

Cited by 148 publications

References 3 publications

Non-LTE modelling of prominence fine structures using hydrogen Lyman-line profiles

Non-LTE modelling of prominence fine structures using hydrogen Lyman-line profiles

The Interface Region Imaging Spectrograph (IRIS)

HST/STIS high resolution echelle spectra ofαCentauri A (G2 V)

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