Properties of a Sunspot Plume Observed with the Coronal Diagnostic Spectrometer Aboard theSolar and Heliospheric Observatory

2005 ◽  
Vol 632 (2) ◽  
pp. 1196-1203 ◽  
Author(s):  
Jeffrey W. Brosius ◽  
Enrico Landi
Keyword(s):  
Heliospheric Observatory ◽  
Coronal Diagnostic Spectrometer

The Coronal Diagnostic Spectrometer for the Solar and Heliospheric Observatory: experiment description and calibration

Metrologia ◽  
1995 ◽  
Vol 32 (6) ◽  
pp. 647-652 ◽  
Author(s):  
R A Harrison ◽  
B J Kent ◽  
E C Sawyer ◽  
J Hollandt ◽  
M K hne ◽  
...  
Keyword(s):  
Heliospheric Observatory ◽  
Experiment Description ◽  
Coronal Diagnostic Spectrometer

The Coronal Diagnostic Spectrometer for the Solar and Heliospheric Observatory

1995 ◽  
pp. 233-290
Author(s):  
R. A. Harrison ◽  
E. C. Sawyer ◽  
M. K. Carter ◽  
A. M. Cruise ◽  
R. M. Cutler ◽  
...  
Keyword(s):  
Heliospheric Observatory ◽  
Coronal Diagnostic Spectrometer

The Coronal Diagnostic Spectrometer for the solar and heliospheric observatory

Solar Physics ◽  
1995 ◽  
Vol 162 (1-2) ◽  
pp. 233-290 ◽  
Author(s):  
R. A. Harrison ◽  
E. C. Sawyer ◽  
M. K. Carter ◽  
A. M. Cruise ◽  
R. M. Cutler ◽  
...  
Keyword(s):  
Heliospheric Observatory ◽  
Coronal Diagnostic Spectrometer

scholarly journals The Temperature of the Extended Solar Corona

2001 ◽  
Vol 203 ◽  
pp. 505-507
Author(s):  
C. R. Foley ◽  
J. L. Culhane ◽  
D. MacKay
Keyword(s):  
Solar Corona ◽  
Electron Temperature ◽  
Solar Minimum ◽  
Solar Maximum ◽  
Radial Variation ◽  
Heliospheric Observatory ◽  
Coronal Diagnostic Spectrometer

We use the Coronal Diagnostic Spectrometer instrument on board the Solar and Heliospheric Observatory to analyse coronal helmet streamer structures observed close to the solar minimum / maximum on the 1996 July 8 / 1999 August 4-5th. The radial variation of peak electron temperature is extracted out to 2 solar radii. These are found to agree well with Yohkoh observations close to the solar maximum, but are found to be reduced by around half a million close to the solar minimum.

Coronal Diagnostic Spectrometer: an extreme-ultraviolet spectrometer for the Solar and Heliospheric Observatory

1995 ◽  
Author(s):  
Barry J. Kent ◽  
Richard A. Harrison ◽  
Eric C. Sawyer ◽  
R. W. Hayes ◽  
Anthony G. Richards ◽  
...  
Keyword(s):  
Extreme Ultraviolet ◽  
Heliospheric Observatory ◽  
Ultraviolet Spectrometer ◽  
Coronal Diagnostic Spectrometer

scholarly journals The Solar and Heliospheric Observatory

1984 ◽  
Vol 86 ◽  
pp. 155-158 ◽  
Author(s):  
Giancarlo Noci
Keyword(s):  
Solar Physics ◽  
Grazing Incidence ◽  
Spectral Irradiance ◽  
The Sun ◽  
Solar Dynamics Observatory ◽  
Solar Constant ◽  
Heliospheric Observatory ◽  
Explorer Mission ◽  
Solar Dynamics ◽  
Euv Spectrum

In the past years several space missions have been proposed for the study of the Sun and of the Heliosphere. These missions were intended to clarify various different aspects of solar physics. For example, the GRIST (Grazing Incidence Solar Telescope) mission was intended as a means to improve our knowledge of the upper transition region and low corona through the detection of the solar EUV spectrum with a spatial resolution larger than in previous missions; the DISCO (Dual Spectral Irradiance and Solar Constant Orbiter) and SDO (Solar Dynamics Observatory) missions were proposed to gat observational data about the solar oscillations better than those obtained from ground based instruments; the SOHO (Solar and Heliospheric Observatory) mission was initially proposed to combine the properties of GRIST with the study of the extended corona (up to several radii of heliocentric distance) by observing the scattered Ly-alpha and OVI radiation, which was also the basis of the SCE (Solar Corona Explorer) mission proposal; the development of the interest about the variability of the Sun, both in itself and for its consequences in the history of the Earth, led to propose observations of the solar constant (included in DISCO).

scholarly journals The Balloon-Borne Investigation of Temperature and Speed of Electrons in the Corona (BITSE): Mission Description and Preliminary Results

Solar Physics ◽  
2021 ◽  
Vol 296 (1) ◽  
Author(s):  
N. Gopalswamy ◽  
J. Newmark ◽  
S. Yashiro ◽  
P. Mäkelä ◽  
N. Reginald ◽  
...  
Keyword(s):  
Heliocentric Distance ◽  
Signal To Noise Ratio ◽  
Flow Speed ◽  
Science Data ◽  
Uncertainty Interval ◽  
Heliospheric Observatory ◽  
Flash Storage ◽  
Goddard Space Flight Center ◽  
Good Agreement ◽  
Polarization Camera

AbstractWe report on the Balloon-borne Investigation of Temperature and Speed of Electrons in the corona (BITSE) mission launched recently to observe the solar corona from $\approx 3$ ≈ 3  Rs to 15 Rs at four wavelengths (393.5, 405.0, 398.7, and 423.4 nm). The BITSE instrument is an externally occulted single stage coronagraph developed at NASA’s Goddard Space Flight Center in collaboration with the Korea Astronomy and Space Science Institute (KASI). BITSE used a polarization camera that provided polarization and total brightness images of size $1024 \times 1024$ 1024 × 1024 pixels. The Wallops Arc Second Pointer (WASP) system developed at NASA’s Wallops Flight Facility (WFF) was used for Sun pointing. The coronagraph and WASP were mounted on a gondola provided by WFF and launched from the Fort Sumner, New Mexico station of Columbia Scientific Balloon Facility (CSBF) on September 18, 2019. BITSE obtained 17,060 coronal images at a float altitude of $\approx \mbox{128,000}$ ≈ 128,000 feet ($\approx 39$ ≈ 39  km) over a period of $\approx 4$ ≈ 4  hrs. BITSE flight software was based on NASA’s core Flight System, which was designed to help develop flight quality software. We used EVTM (Ethernet Via Telemetry) to download science data during operations; all images were stored on board using flash storage. At the end of the mission, all data were recovered and analyzed. Preliminary analysis shows that BITSE imaged the solar minimum corona with the equatorial streamers on the east and west limbs. The narrow streamers observed by BITSE are in good agreement with the geometric properties obtained by the Solar and Heliospheric Observatory (SOHO) coronagraphs in the overlapping physical domain. In spite of the small signal-to-noise ratio ($\approx 14$ ≈ 14 ) we were able to obtain the temperature and flow speed of the western steamer. In the heliocentric distance range 4 – 7 Rs on the western streamer, we obtained a temperature of $\approx 1.0\pm 0.3$ ≈ 1.0 ± 0.3  MK and a flow speed of $\approx 260$ ≈ 260  km s−1 with a large uncertainty interval.

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