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Bogong moths navigate using a light-dependent geomagnetic inclination compass
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Magnetic Activity in Cool Stars
Space Science Reviews, 1985Aspects of magnetic activity of late-type stars are reviewed: first, results obtained through the comparison of emissions from various temperature regimes in the outer atmospheres of cool stars, then results from stellar soft X-ray spectroscopy. Spectra obtained with different instruments (Imaging Proportional Counter and Solid State Spectrometer ...
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Nature, 1965
X-ray emission and cooling of neutron stars, combining neutrino emission from interior and photon emission from ...
SACHIKO TSURUTA, A. G. W. CAMERON
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X-ray emission and cooling of neutron stars, combining neutrino emission from interior and photon emission from ...
SACHIKO TSURUTA, A. G. W. CAMERON
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Advances in Space Research, 1983
The consequences of magnetic fields for the atmospheres of cool stars are addressed based on IUE and Einstein Observatory observations. Gross atmospheric structure data for cool luminous stars are discussed, and the relevance of the observations for the energy balance and nonradiative heating rates is considered.
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The consequences of magnetic fields for the atmospheres of cool stars are addressed based on IUE and Einstein Observatory observations. Gross atmospheric structure data for cool luminous stars are discussed, and the relevance of the observations for the energy balance and nonradiative heating rates is considered.
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On the cooling of neutron stars
Journal of Physics G: Nuclear and Particle Physics, 1995It has recently been pointed out that many models of dense nuclear matter allow the direct URCA process in highly dense systems like neutron stars. In view of this, we have calculated the energy loss in dense nuclear matter as a result of such processes at finite temperatures.
A Wadhwa, V K Gupta, S Singh, J D Anand
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Astrophysics and Space Science, 1971
With the hypothesis generally adopted as responsible for the heating of the solar corona an attempt was made to predict the coronal temperature for a few cool stars. Stars with effective temperatures between 2500K and 3700K, with logg-values of 3 or 4, appear to have coronal temperatures only 600 to 25000K higher thanT eff.
C. de Jager, C. de Loore
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With the hypothesis generally adopted as responsible for the heating of the solar corona an attempt was made to predict the coronal temperature for a few cool stars. Stars with effective temperatures between 2500K and 3700K, with logg-values of 3 or 4, appear to have coronal temperatures only 600 to 25000K higher thanT eff.
C. de Jager, C. de Loore
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Astrophysics and Space Science, 1990
If we follow recent work and in order to extend theuvby photometric calibrations to spectral types later than G0, we present an attempt to use the combineduvby andβ systems for stars in the range G5-K7 and luminosity classes V to III.
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If we follow recent work and in order to extend theuvby photometric calibrations to spectral types later than G0, we present an attempt to use the combineduvby andβ systems for stars in the range G5-K7 and luminosity classes V to III.
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Facular structures on cool stars
1999Activity has many manifestations, from dark spots to bright regions, to the presence of the heated chromosphere, to the superheated corona. Sunspots are extended, strongly magnetic regions on the Sun. Photospheric faculae are generally visible only at the limb. Polar faculae are smaller than the main-zone faculae. the contributions of the active region
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Reviews of Modern Physics, 1992
A review is given of the important neutrino emission processes in neutron star interiors, and their consequences for the cooling of neutron stars.
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A review is given of the important neutrino emission processes in neutron star interiors, and their consequences for the cooling of neutron stars.
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