Hostname: page-component-848d4c4894-cjp7w Total loading time: 0 Render date: 2024-06-29T02:50:21.987Z Has data issue: false hasContentIssue false
  • English
  • Français

Cooling of Dense Stars

Published online by Cambridge University Press:  14 August 2015

Sachiko Tsuruta
Sachiko Tsuruta*
Affiliation:
NASA, Goddard Space Flight Center, Greenbelt, Md., U.S.A.

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Cooling rates are first calculated for neutron stars of about 1 M⊙ and 10 km radius, with magnetic fields from zero to about 1014 G, for two extreme cases of maximum and no superfluidity. The results show that most pulsars are so cold that thermal ionization of surface atoms would be negligible. Next, nucleon superfluidity and crystallization of heavy nuclei are treated more quantitatively, and more realistic hadron star models are chosen. Cooling rates are thus calculated for a stable hyperon star near the maximum mass limit, a medium weight neutron star, and a light neutron star with neutron-rich heavy nuclei near the minimum mass limit. Results show that cooling rates are a sensitive function of density. The lightest star is cooler than others in earlier stages but the trend is reversed later. The medium weight star is generally the coldest of all in lower temperature regions where the effect of superfluidity becomes significant. However, if a heavy star contains pions, its cooling will be even faster. The Crab pulsar and Vela pulsar, expected to be the two youngest, can be as hot as (2 ∼ 4) x 106 K (on the surface), comparable with the results obtained from internal frictional heating by Greenstein, if they are medium weight to heavy hadron stars. However, older pulsars are cold. In fact, at about a few million years, the age of average radio pulsars, the surface temperature becomes only several hundred to several thousand degrees. Thus, the earlier conclusions about cold pulsars are still valid. Cooling of a massive white dwarf star is also shown.

Type
Research Article
Information
Symposium - International Astronomical Union , Volume 53: Physics of Dense Matter , 1974 , pp. 209 - 225
Copyright
Copyright © Reidel 1974 

References

Bahcall, J. N. and Wolf, R. A.: 1965a, Phys. Rev. 140, B1452.Google Scholar
Bahcall, J. N. and Wolf, R. A.: 1965b, Phys. Rev. Letters 14, 343.Google Scholar
Baym, G., Bethe, H. A., and Pethick, C. J.: 1971a, Nucl. Phys. A175, 225.Google Scholar
Baym, G., Pethick, C. J., and Sutherland, P.: 1971b, Astrophys. J. 170, 299.Google Scholar
Beaudet, G., Petrosian, V., and Salpeter, E. E.: 1967, Astrophys. J. 150, 979.Google Scholar
Bethe, H. A.: 1972 (private communication).Google Scholar
Borner, G. and Cohen, J. M.: 1972, Pulsar Speed-ups (preprint).Google Scholar
Cameron, A. G. W.: 1970 (private communication).Google Scholar
Canuto, V.: 1970, Astrophys. J. 160, L153.CrossRefGoogle Scholar
Canuto, V. and Chiu, H.-Y.: 1969, Phys. Rev. 188, 2446.Google Scholar
Canuto, V., Lodenquai, J., and Ruderman, M.: 1971, Phys. Rev. D3, 2303.Google Scholar
Cohen, J. M. and Borner, G.: 1972 (private communication).Google Scholar
Ginzburg, V. L.: 1971, Physica 55, 207.Google Scholar
Gold, T.: 1968, Nature 218, 731.CrossRefGoogle Scholar
Greenstein, G.: 1971, Nature Phys. Sci. 232, 117.Google Scholar
Gunn, J. E. and Ostriker, J. P.: 1970, Astrophys. J. 160, 979.Google Scholar
Hansen, C. J.: 1968, Astrophys. Space Sci. 1, 499.Google Scholar
Hartle, J. B. and Thorne, K. S.: 1968, Astrophys. J. 153, 807.Google Scholar
Ikeuchi, S., Nagata, S., Mizutani, T., and Nakazawa, K.: 1971, Prog. Theor. Phys. 46, 95.Google Scholar
Itoh, N.: 1971 (private communication).Google Scholar
Itoh, N. and Tsuneto, T.: 1972, Prog. Theor. Phys. Kyoto 48, 1849.Google Scholar
Landau, L. D. and Lifshitz, E. M.: 1958, Statistical Physics, Addison-Wesley Publ. Co., Mass. Google Scholar
Lodenquai, J., Canuto, V., Ruderman, M., and Tsuruta, S.: 1974 (to be published).Google Scholar
Mestel, L. and Ruderman, M.: 1967, Monthly Notices Roy. Astron. Soc. 136, 27.CrossRefGoogle Scholar
Moszkowski, S. A.: 1972, paper presented at APS Meeting, April, Washington D. C. (Bulletin of APS 17, 502).Google Scholar
Pandharipande, V. R.: 1971, Nucl. Phys. A178, 123.Google Scholar
Ravenhall, D. G., Bennett, C. D., and Pethick, C. J.: 1972, Nuclear Surface Energy and Neutron Star Matter (preprint), (1972, Phys. Rev. Letters 28, 978).Google Scholar
Ruderman, M.: 1971, Phys. Rev. Letters 27, 1306.CrossRefGoogle Scholar
Salpeter, E. E.: 1961, Astrophys. J. 134, 669.Google Scholar
Sawyer, R. F.: 1972, Phys. Rev. Letters 29, 382.Google Scholar
Scalapino, D. J.: 1972, Phys. Rev. Letters 29, 386.Google Scholar
Schatzman, E.: 1958, White Dwarfs, North-Holland Publ. Co, Amsterdam.Google Scholar
Shaham, J.: 1972 (private communication).Google Scholar
Tamagaki, R.: 1968, Prog. Theor. Phys. Kyoto 39, 91.Google Scholar
Tamagaki, R.: 1972 (private communication).Google Scholar
Takatsuka, T.: 1972, Energy Gap in Neutron-Star Matter (preprint) NEAP-11, May, Kyoto University, (1972, Prog. Theor. Phys. Kyoto 48, 1517).Google Scholar
Tsuruta, S.: 1964, .Google Scholar
Tsuruta, S.: 1974 (to be published).Google Scholar
Tsuruta, S. and Cameron, A. G. W.: 1966a, Can. J. Phys. 44, 1863.Google Scholar
Tsuruta, S. and Cameron, A. G. W.: 1966b, Can. J. Phys. 44, 1895.Google Scholar
Tsuruta, S. and Cameron, A. G. W.: 1970, Astrophys. Space Sci. 7, 374.Google Scholar
Tsuruta, S., Canuto, V., Lodenquai, J., and Ruderman, M.: 1972, Astrophys. J. 176, 739.Google Scholar
Tsuruta, S., Truran, J. W., and Cameron, A. G. W.: 1973, Bulletin of APS 18, 541.Google Scholar
Van Horn, H. M.: 1968, Astrophys. J. 151, 227.CrossRefGoogle Scholar
Wheeler, J. A.: 1966, Ann. Rev. Astron. Astrophys. 4, 393.Google Scholar
Wolf, R. A. 1966, Astrophys. J. 145, 834.CrossRefGoogle Scholar