October 1965
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9 Reads
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32 Citations
Physical Review Letters
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Publications (2)
January 1965
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6 Reads
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25 Citations
Physical Review
The energy loss of a degenerate neutron gas by the "Urca" process is calculated in this paper; it is 7.36×104(T/109)8 erg g-1 for a density of 6×1014 g cm-3. It follows from this energy loss that the Urca process alone should have cooled the core of the neutron star created in the type I supernova of 1054 a.d. to a temperature around 5×108 °K. The emission power of the star should then be about one order of magnitude smaller than that of the x-ray source discovered recently in the Crab nebula; the source cannot be interpreted therefore simply as the thermal radiation of the star. This conclusion is consistent with the result of a recent experiment performed by the method of lunar occultation, indicating an angular size of the source comparable to that of the Crab nebula. A more refined experiment performed by the same method should, on the other hand, make it possible to decide whether a neutron star exists in the Crab nebula.
Citations (2)
... They wrote that their estimate of the neutrino energy loss was "essentially the result of a dimensional analysis and could be in error by several orders of magnitude." Then followed calculations by other authors [19][20][21][22]. The series of pioneer articles of 1964-1965 was concluded with a detailed paper by Bahcall and Wolf [16] who also critically reviewed previous calculations of the Murca cooling rate. ...
- Citing Article
January 1965
Physical Review
... In the mid-1960s, researchers were interested in the radial oscillation modes of neutron stars presumed to arise in their initial formation in supernovae. Curiosity about the duration of these oscillations after the birth of the neutron star, as well as the possibility of the conversion of vibrational energy into heat, leading to enhanced radiation from the neutron star surface (see the contemporary review articles [21,22]), lead to preliminary calculations (Finzi [23], Meltzer & Thorne [24], and Hansen & Tsuruta [25]) of vibrational energy dissipation arising from chemical equilibration. In these early works, which considered neutron stars built of neutron-proton-electron (npe) matter (see Sec. II), modified Urca processes (Sec. ...
Reference:
Bulk Viscosity in Dense Nuclear Matter
- Citing Article
October 1965
Physical Review Letters