Flare stars and solar bursts: High resolution in time and frequency

Solar Physics ◽  
1986 ◽  
Vol 104 (1) ◽  
pp. 227-233 ◽  
Author(s):  
Kenneth R. Lang
Keyword(s):  
High Resolution ◽  
Flare Stars ◽  
Solar Bursts

High-resolution microwave spectra of solar bursts

Solar Physics ◽  
1989 ◽  
Vol 120 (2) ◽  
pp. 351-368 ◽  
Author(s):  
M. St�hli ◽  
D. E. Gary ◽  
G. J. Hurford
Keyword(s):  
High Resolution ◽  
Microwave Spectra ◽  
Solar Bursts

A self-adaptive method for the determination of solar bursts for high-resolution solar radio spectrometer

2019 ◽  
Vol 364 (6) ◽  
Author(s):  
Qing-Fu Du ◽  
Chang-Shuo Chen ◽  
Qiao-Man Zhang ◽  
Xin Li ◽  
Yong Song
Keyword(s):  
High Resolution ◽  
Solar Radio ◽  
Adaptive Method ◽  
Solar Bursts ◽  
Radio Spectrometer ◽  
Self Adaptive

Recent and Future Radio Observations of Flare Stars

1979 ◽  
Vol 46 ◽  
pp. 150-160
Author(s):  
O.B. Slee ◽  
A.A. Page
Keyword(s):  
Angular Resolution ◽  
Selection Effect ◽  
Flare Star ◽  
Optical Studies ◽  
Positive Identification ◽  
The Poor ◽  
Typical Event ◽  
Flare Stars ◽  
Solar Bursts ◽  
Optical Flare

Observations of flare stars began in Australia in 1962 soon after the commissioning of the Parkes 64-m reflector, which was successfully used to detect 408 MHz emission from V371 Orionis during an optical flare; this result was published by Slee et al. (1963) shortly after Lovell et al. (1963) reported their first successful observations of UV Ceti at 240 MHz. Thereafter a number of cooperative radio and optical studies were made with the large reflectors at Jodrell Bank and Parkes and more recently at Arecibo. Unfortunately the poor angular resolution (1° to 2°) of these large single reflectors at metre wavelengths did not permit the positioning of a weak radio source with an accuracy sufficient for positive identification of flare star emission - the observer had to rely on the presence of an optical flare to distinguish the flare deflections on the radio record from interference and baseline drifts. Naturally this resulted in general scepticism among astronomers concerning the reality of the flare star radio emission, especially as the radio luminosity of a typical event was shown to be several orders of magnitude higher than the most intense solar bursts. In addition, it is clear that the method of observing strongly favoured the detection of the shorter impulsive type of bursts lasting from seconds to a few minutes - this selection effect resulted from the difficulty in discriminating between weak, slowly varying flare-star emission and changes in the receiver baseline due to receiver instability.

High resolution observations of solar bursts at 3.7 and 11.1 cm wavelengths

Solar Physics ◽  
1975 ◽  
Vol 41 (1) ◽  
pp. 119-133 ◽  
Author(s):  
C. E. Alissandrakis ◽  
M. R. Kundu
Keyword(s):  
High Resolution ◽  
Solar Bursts

Observations of the spatial structure of interstellar hydrogen

1967 ◽  
Vol 31 ◽  
pp. 45-46
Author(s):  
Carl Heiles
Keyword(s):  
High Resolution ◽  
Spatial Structure ◽  
Velocity Dispersion ◽  
Temperature Variations

High-resolution 21-cm line observations in a region aroundlII= 120°,b11= +15°, have revealed four types of structure in the interstellar hydrogen: a smooth background, large sheets of density 2 atoms cm-3, clouds occurring mostly in groups, and ‘Cloudlets’ of a few solar masses and a few parsecs in size; the velocity dispersion in the Cloudlets is only 1 km/sec. Strong temperature variations in the gas are in evidence.

Combining integrated systems-biology approaches with intervention-based experimental design provides a higher-resolution path forward for microbiome research

2019 ◽  
Vol 42 ◽  
Author(s):  
J. Alfredo Blakeley-Ruiz ◽  
Carlee S. McClintock ◽  
Ralph Lydic ◽  
Helen A. Baghdoyan ◽  
James J. Choo ◽  
...  
Keyword(s):  
Systems Biology ◽  
High Resolution ◽  
Experimental Design ◽  
Integrated Systems ◽  
Microbiome Research ◽  
Constructive Criticism

Abstract The Hooks et al. review of microbiota-gut-brain (MGB) literature provides a constructive criticism of the general approaches encompassing MGB research. This commentary extends their review by: (a) highlighting capabilities of advanced systems-biology “-omics” techniques for microbiome research and (b) recommending that combining these high-resolution techniques with intervention-based experimental design may be the path forward for future MGB research.

Very High Resolution Analysis of the Dynamics of a Coronal Plasmoid

1994 ◽  
Vol 144 ◽  
pp. 593-596
Author(s):  
O. Bouchard ◽  
S. Koutchmy ◽  
L. November ◽  
J.-C. Vial ◽  
J. B. Zirker
Keyword(s):  
High Resolution ◽  
Solar Eclipse ◽  
Total Solar Eclipse ◽  
Field Of View ◽  
Small Field ◽  
High Resolution Analysis ◽  
Ccd Observations ◽  
Resolution Analysis ◽  
Very High ◽  
Small Field Of View

AbstractWe present the results of the analysis of a movie taken over a small field of view in the intermediate corona at a spatial resolution of 0.5“, a temporal resolution of 1 s and a spectral passband of 7 nm. These CCD observations were made at the prime focus of the 3.6 m aperture CFHT telescope during the 1991 total solar eclipse.

FeXIV Line Emission Polarization of the July 11, 1991 Solar Corona

1994 ◽  
Vol 144 ◽  
pp. 541-547
Author(s):  
J. Sýkora ◽  
J. Rybák ◽  
P. Ambrož
Keyword(s):  
High Resolution ◽  
Solar Corona ◽  
Emission Line ◽  
Solar Eclipse ◽  
White Light ◽  
Preliminary Analysis ◽  
Line Emission ◽  
Total Solar Eclipse ◽  
Degree Of Polarization ◽  
High Resolution Images

AbstractHigh resolution images, obtained during July 11, 1991 total solar eclipse, allowed us to estimate the degree of solar corona polarization in the light of FeXIV 530.3 nm emission line and in the white light, as well. Very preliminary analysis reveals remarkable differences in the degree of polarization for both sets of data, particularly as for level of polarization and its distribution around the Sun’s limb.

Microcalorimeters for X-Ray Spectroscopy

1988 ◽  
Vol 102 ◽  
pp. 41
Author(s):  
E. Silver ◽  
C. Hailey ◽  
S. Labov ◽  
N. Madden ◽  
D. Landis ◽  
...  
Keyword(s):  
High Resolution ◽  
High Efficiency ◽  
Thermal Response ◽  
Low Noise ◽  
High Resolution Spectroscopy ◽  
Superconducting Transition ◽  
Sapphire Substrates ◽  
Laboratory Plasmas ◽  
Adiabatic Demagnetization ◽  
Theoretical Predictions

The merits of microcalorimetry below 1°K for high resolution spectroscopy has become widely recognized on theoretical grounds. By combining the high efficiency, broadband spectral sensitivity of traditional photoelectric detectors with the high resolution capabilities characteristic of dispersive spectrometers, the microcalorimeter could potentially revolutionize spectroscopic measurements of astrophysical and laboratory plasmas. In actuality, however, the performance of prototype instruments has fallen short of theoretical predictions and practical detectors are still unavailable for use as laboratory and space-based instruments. These issues are currently being addressed by the new collaborative initiative between LLNL, LBL, U.C.I., U.C.B., and U.C.D.. Microcalorimeters of various types are being developed and tested at temperatures of 1.4, 0.3, and 0.1°K. These include monolithic devices made from NTD Germanium and composite configurations using sapphire substrates with temperature sensors fabricated from NTD Germanium, evaporative films of Germanium-Gold alloy, or material with superconducting transition edges. A new approache to low noise pulse counting electronics has been developed that allows the ultimate speed of the device to be determined solely by the detector thermal response and geometry. Our laboratory studies of the thermal and resistive properties of these and other candidate materials should enable us to characterize the pulse shape and subsequently predict the ultimate performance. We are building a compact adiabatic demagnetization refrigerator for conveniently reaching 0.1°K in the laboratory and for use in future satellite-borne missions. A description of this instrument together with results from our most recent experiments will be presented.

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