Zobrazeno 1 - 10
of 943
pro vyhledávání: '"Schlattl H"'
Autor:
Kunert P; Department of Medical and Occupational Radiation Protection, Federal Office for Radiation Protection, Oberschleißheim, Germany., Schlattl H; Department of Medical and Occupational Radiation Protection, Federal Office for Radiation Protection, Oberschleißheim, Germany., Trinkl S; Department of Medical and Occupational Radiation Protection, Federal Office for Radiation Protection, Oberschleißheim, Germany., Honorio da Silva E; Department of Medical and Occupational Radiation Protection, Federal Office for Radiation Protection, Oberschleißheim, Germany., Reichert D; Department of Physics, Martin-Luther University Halle-Wittenberg, Halle (Saale), Germany., Giussani A; Department of Medical and Occupational Radiation Protection, Federal Office for Radiation Protection, Oberschleißheim, Germany.
Publikováno v:
Medical physics [Med Phys] 2024 Dec; Vol. 51 (12), pp. 9264-9274. Date of Electronic Publication: 2024 Sep 19.
Publikováno v:
Astron.Astrophys.411:1129-1133,2003
Two key reactions of hydrostatic nuclear burning in stars have recently been revised by new experimental data - the 14N(p,gamma)15O and triple alpha reaction rates. We investigate how much the new rates influence the evolution of low-mass, metal-poor
Externí odkaz:
http://arxiv.org/abs/astro-ph/0503408
Autor:
de las Heras Gala, H., Schöfer, F., Schöfer, H., Sánchez Casanueva, R.M., Zervides, C., Mair, K., Al-Zoubi, Q., Renger, B., de las Heras Gala, T., Schlattl, H.
Publikováno v:
In Physica Medica March 2018 47:92-102
Publikováno v:
Astron.Astrophys. 422 (2004) 217-223
Two alternative scenarios concerning the origin and evolution of extremely metal-poor halo stars are investigated. The first one assumes that the stars have been completely metal-free initially and produced observed carbon and nitrogen overabundances
Externí odkaz:
http://arxiv.org/abs/astro-ph/0402334
Publikováno v:
Astrophys.Space Sci.291:27-56,2004
We investigate the dependence of the carbon and oxygen production in stars on the 3-alpha rate by varying the energy of the 02+-state of 12C and determine the resulting yields for a selection of low-mass, intermediate-mass, and massive stars. The yie
Externí odkaz:
http://arxiv.org/abs/astro-ph/0307528
Autor:
Schlattl, H., Salaris, M.
Publikováno v:
Astron.Astrophys. 402 (2003) 29-36
We review the state of the art regarding the computation of the resistance coefficients in conditions typical of the stellar plasma, and compare the various results studying their effect on the solar model. We introduce and discuss for the first time
Externí odkaz:
http://arxiv.org/abs/astro-ph/0302353
Publikováno v:
Astrophys.J. 582 (2003) L43-L46
The core helium-flash in low-mass stars with extreme mass loss occurs after the tip of the RGB, when the H-rich envelope is very thin. The low efficiency of the H-shell source enables the He-flash driven convective zone to penetrate H-rich layers and
Externí odkaz:
http://arxiv.org/abs/astro-ph/0211498
Publikováno v:
Nucl.Phys. A719 (2003) 283-286
We investigate the triple-alpha process and the Oklo phenomenon to obtain constraints on possible cosmological time variations of fundamental constants. Specifically we study cosmological temporal constraints for the fine structure constant and nucle
Externí odkaz:
http://arxiv.org/abs/astro-ph/0210459
Autor:
Schlattl, H.
Publikováno v:
Astron.Astrophys. 395 (2002) 85
An improved microscopic diffusion in stars is presented considering in detail the partly ionized stages of metals. Besides,the influence of degenerate electron-gas and of the contribution of radiation to the total pressure has been accounted for. The
Externí odkaz:
http://arxiv.org/abs/astro-ph/0208473
Publikováno v:
Astron.Astrophys. 395 (2002) 77-84
We investigate whether the observed high number of carbon- and nitrogen-enhanced extremely metal-poor stars could be explained by peculiar evolutionary properties during the core He flash at the tip of the red giant branch. For this purpose we comput
Externí odkaz:
http://arxiv.org/abs/astro-ph/0205326