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  • ASTROPHYSICS  (4)
  • 68-501; Ammonium; Calcium; Deep Sea Drilling Project; DEPTH, sediment/rock; DRILL; Drilling/drill rig; DSDP; DSDP/ODP/IODP sample designation; Glomar Challenger; Leg68; Lithium; Magnesium; Manganese; North Pacific/FLANK; Potassium; Sample code/label; Silicate; Sodium; Strontium; Sulfate  (1)
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  • 1
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    Interstitial water chemistry of Hole 68-501 (2005)
    PANGAEA
    Details
    Publication Date: 2023-06-27
    Keywords: 68-501; Ammonium; Calcium; Deep Sea Drilling Project; DEPTH, sediment/rock; DRILL; Drilling/drill rig; DSDP; DSDP/ODP/IODP sample designation; Glomar Challenger; Leg68; Lithium; Magnesium; Manganese; North Pacific/FLANK; Potassium; Sample code/label; Silicate; Sodium; Strontium; Sulfate
    Type: Dataset
    Format: text/tab-separated-values, 92 data points
    Location Call Number Expected Availability
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    DATA PANGAEA
  • 2
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    Radio constraints on coronal models for dMe stars (1994)
    In:  Other Sources
    Details
    Publication Date: 2019-07-13
    Description: Radio data are used to test coronal models for dMe stars. Specifically, we show that photospheric magnetic field observations imply that the low corona of a dMe star should be saturated by magnetic fields with an average strength in excess of 1 kG. In such fields the hot component of the corona detected in X-ray observations (temperature of order 2 x 10(exp 7) K) would be optically thick at least up to 15 GHz due to thermal gyroresonance opacity. The resulting emission would easily be detectable by radio observations and should have a radio spectrum rising in the microwave range. We have carried out observations to test this prediction, and in the majority of cases find that the observed fluxes at 15 GHz are too low to be consistent with the assumptions. In the few cases where the stars were detected at 15 GHz, the evidence indicates that the observed emission is nonthermal. These results imply that the hot component of the X-ray-emitting plasma in the corona is not coincident with the strong magnetic fields in the lower corona. Because the hot plasma must still be confined by closed magnetic field lines, it is likely to be restricted to heights of the order of a stellar radius above the photosphere. The results seem to imply a different genesis for the two components of the X-ray-emitting corona of flare stars: the hot component may be cooling flare plasma, while the cooler component (temperature of order 3 x 10(exp 6) K) is associated with a more conventional coronal heating mechanism.
    Keywords: ASTROPHYSICS
    Type: Astrophysical Journal, Part 1 (ISSN 0004-637X); 422; 1; p. 293-303
    Format: text
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    NASA TECHNICAL REPORTS
  • 3
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    Nonthermal processes in flaring X-ray-bright points (1994)
    In:  Other Sources
    Details
    Publication Date: 2019-08-28
    Description: X-ray-bright point (XBPs) are known to show variability on a number of timescales, including impulsive X-ray brightenings. The relationship between these XBP 'flares' and normal solar flares is poorly known. A fundamental question is whether nonthermal acceleration of particles takes place in XBP flares. We address this issue by searching for nonthermal radio emission at metric wavelengths from flaring XBPs identified in Yohkoh soft x-ray telescope (SXT) data. Unequivocal evidence for type III-like radio bursts, usually attributed to beams of nonthermal electrons on open field lines, is found. This suggests that XBP flares are similar to normal flares and can indeed accelerate nonthermal populations of energetic particles.
    Keywords: ASTROPHYSICS
    Type: Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X); 427; 1; p. L59-L62
    Format: text
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    NASA TECHNICAL REPORTS
  • 4
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    Radio observations of solar and stellar coronae (1992)
    In:  Other Sources
    Details
    Publication Date: 2019-07-13
    Description: Recent results of radio observations of the solar and stellar coronae are reviewed. Attention is given to the results obtained on quiet-sun fine structures; the active region observations, with particular consideration given to the soft X-ray and radio comparisons of observations made during the Coronal Magnetic Structures Observing Campaign and the strength of the magnetic fields in the corona; the radio observations of solar flares; and the radio observations of stellar coronae of the RS Canum Venaticorum binaries, M dwarf stars, pre-main-sequence stars, and chemically-peculiar B stars. Also discussed are current issues in stellar radiophysics and perspectives in solar radio physics.
    Keywords: ASTROPHYSICS
    Type: Societa Astronomica Italiana, Memorie (ISSN 0037-8720); 63; 4-Mar; p. 715-730.
    Format: text
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    NASA TECHNICAL REPORTS
  • 5
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    Microwave observations of the flare stars UV Ceti, AT Microscopii, and AU Microscopii (1987)
    In:  Other Sources
    Details
    Publication Date: 2019-07-12
    Description: The results of observations of three red dwarf flare star systems, UV Ceti, AT Mic, and AU Mic, made in February and March of 1985, are reported. Flaring was detected from all three systems, and quiescent emission from UV Cet and AU Mic. Models for the quiescent microwave-emitting corona of UV Cet are discussed. The gravitational scale height in current models is similar to or larger than the height of the corona, which is a striking difference from the case of the solar corona and confirms that magnetic structures are required to confine the radio-emitting corona. The role of precipitation into the chromosphere of the energetic particles in such a corona is explored, and it is shown that for plausible parameters it may be the dominant energy loss mechanism.
    Keywords: ASTROPHYSICS
    Type: Astrophysical Journal, Part 1 (ISSN 0004-637X); 312; 822-829
    Format: text
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    NASA TECHNICAL REPORTS
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