Abstract
The neutrino cooling and gamma heating rates are considered as an important input needed to study the final phases of the evolution of high-mass stars. The weak-interaction mediated processes, namely the \(\beta \)-decay and electron capture, significantly change the lepton to baryon ratio and accelerate the contraction of the core. The emission of resulting neutrinos/antineutrinos tend to cool the stellar core. On the other hand gamma rays are produced because of electron capture and \(\beta \)-decay to excited states in daughter nuclei. These gamma rays heat the core and contribute to increase of entropy which may cause convection to occur. In the present work, the weak-interaction heating and cooling rates on a chain of twenty two isotopes of vanadium having mass in the range 43–64 have been estimated using the proton-neutron quasiparticle random phase approximation theory. The rates have been computed for the temperature ranging from (\(10^{7}\mbox{--}3\times 10^{10}\)) K and for the density range \((10\mbox{--}10^{11})~\mbox{g/cm}^{3}\). Our calculated neutrino energy loss rates have also been compared with the previously reported rates calculated using other theoretical models. At high stellar temperatures, our rates are larger by 1–2 orders of magnitude as compared to previous results.
Similar content being viewed by others
References
Alford, W.P., et al.: Nucl. Phys. A 514, 49 (1990)
Alford, W.P., et al.: Phys. Rev. C 48, 2818 (1993)
Audi, G., et al.: Chin. Phys. C 41, 030001 (2017)
Aufderheide, M.B., Fushiki, I., Woosley, S.E., et al.: Astrophys. J. Suppl. 91, 389 (1994)
Bäumer, C., et al.: Phys. Rev. C 68, 031303(R) (2003)
Bäumer, C., et al.: Phys. Rev. C 71, 024603 (2005)
Bethe, H.A.: Rev. Mod. Phys. 62, 801 (1990)
Bethe, H.A., Brown, G.E., Applegate, J., et al.: Nucl. Phys. A 324, 487 (1979)
Brink, D.: D. Phil. Thesis, Oxford University, Unpublished (1955)
Cole, A.L., et al.: Phys. Rev. C 86, 015809 (2012)
El-Kateb, S., et al.: Phys. Rev. C 49, 3128 (1994)
Fifield, L.K., et al.: Nucl. Phys. A 204, 516–522 (1973)
Fuller, G.M., Fowler, W.A., Newman, M.J.: Astrophys. J. Suppl. Ser. 42, 447 (1980)
Fuller, G.M., Fowler, W.A., Newman, M.J.: Astrophys. J. Suppl. Ser. 48, 279 (1982a)
Fuller, G.M., Fowler, W.A., Newman, M.J.: Astrophys. J. 252, 715 (1982b)
Fuller, G.M., Fowler, W.A., Newman, M.J.: Astrophys. J. 293, 1 (1985)
Gaarde, C.: Nucl. Phys. A 396, 127c (1983)
Giannaka, P.G., Kosmas, T.S.: Adv. High Energy Phys. 2015, 398796 (2015)
Gove, N.B., Martin, M.J.: At. Data Nucl. Data Tables 10, 205 (1971)
Gupta, S., et al.: Astrophys. J. 662(2), 1188 (2007)
Hagberg, E., et al.: Nucl. Phys. A 613, 183 (1997)
Hardy, J.C., Towner, I.C.: Phys. Rev. C 79(5), 055502 (2009)
Heger, A., et al.: Phys. Rev. Lett. 86, 1678 (2001)
Hirsch, M., et al.: Nucl. Phys. 535, 62 (1991)
Hirsch, M., et al.: At. Data Nucl. Data Tables 53, 165–193 (1993)
Hitt, G.W., Gupta, S., Zegers, R.G.T., et al.: arXiv:1610.06992 [nucl-ex], 22 October (2016)
Honma, M., Otsuka, T., Brown, B., Mizusaki, T.: Eur. Phys. J. A 25, 499 (2005)
Ikeda, K., Fujii, S., Fujita, J.I.: Phys. Lett. 3, 271 (1963)
Janka, H.-T., et al.: Phys. Rep. 442, 38 (2007)
José, J., Iliadis, C.: Rep. Prog. Phys. 74(9), 096901 (2011)
Krumlinde, J., Möller, P.: Nucl. Phys. A 417, 419 (1984)
Langanke, K., Martínez-Pinedo, G.: Rev. Mod. Phys. 75, 819 (2003)
Langanke, K., Martínez-Pinedon, G.: Nucl. Phys. A 673, 481 (2000)
Möller, P., et al.: At. Data Nucl. Data Tables 59, 185 (1995)
Möller, P., et al.: At. Data Nucl. Data Tables 66, 131 (1997)
Muto, K., Bender, E., Klapdor, H.V.: Z. Phys. A 333, 125 (1989)
Nabi, J.-U.: Eur. Phys. J. A 40, 223 (2009)
Nabi, J.-U.: Phys. Scr. 81, 025901 (2010a)
Nabi, J.-U.: Int. J. Mod. Phys. E 19, 63 (2010b)
Nabi, J.-U.: Adv. Space Res. 46, 1191 (2010c)
Nabi, J.-U., Klapdor-Kleingrothaus, H.V.: Eur. Phys. J. A 5, 337 (1999)
Nabi, J.-U., Klapdor-Kleingrothaus, H.V.: At. Data Nucl. Data Tables 71, 149 (1999)
Nabi, J.-U., Klapdor-Kleingrothaus, H.V.: At. Data Nucl. Data Tables 88, 237 (2004)
Nabi, J.-U., Sajjad, M.: Phys. Rev. C 76, 055803 (2007)
Nabi, J.-U., Sajjad, M.: Phys. Rev. C 77, 055802 (2008)
Nakamura, K., et al. (Particle Data Group): J. Phys. G, Nucl. Part. Phys. 37(7A), 075021 (2010)
Nilsson, S.G.: Mat.-Fys. Medd. 29, 16 (1955)
Poves, A., et al.: Nucl. Phys. A 694, 157 (2001)
Pruet, J., Fuller, G.M.: Astrophys. J. Suppl. Ser. 149, 189 (2003)
Rahman, M.-U., Nabi, J.-U.: Astrophys. Space Sci. 348, 427–435 (2013)
Rönnqvist, T., et al.: Nucl. Phys. A 563, 225 (1993)
Sarriguren, P.: Phys. Rev. C 87, 045801 (2013)
Sarriguren, P.: Phys. Rev. C 93, 054309 (2016)
Vetterli, M.C., et al.: Phys. Rev. C 40, 559 (1989)
Williams, A.L., et al.: Phys. Rev. C 51, 1144 (1990)
Acknowledgements
J.-U. Nabi would like to acknowledge the support of the Higher Education Commission Pakistan through project numbers 5557/KPK/NRPU/R&D/HEC/2016, 9-5(Ph-1-MG-7)/PAK-TURK/R&D/HEC/2017 and Pakistan Science Foundation through project number PSF-TUBITAK/KP-GIKI (02).
Author information
Authors and Affiliations
Corresponding author
Additional information
Publisher’s Note
Springer Nature remains neutral with regard to jurisdictional claims in published maps and institutional affiliations.
Rights and permissions
About this article
Cite this article
Shehzadi, R., Nabi, JU. & Ali, H. Energy rates due to weak decay rates of vanadium isotopes in stellar environment. Astrophys Space Sci 365, 3 (2020). https://doi.org/10.1007/s10509-019-3716-8
Received:
Accepted:
Published:
DOI: https://doi.org/10.1007/s10509-019-3716-8