Zobrazeno 1 - 10
of 185
pro vyhledávání: '"Lingenfelter R"'
Autor:
Higdon, J. C., Lingenfelter, R. E.
Core collapse supernovae of massive (> 8 Mo) stars are formed primarily in OB associations and help blow giant superbubbles, where their collective shocks accelerate most of the Galactic cosmic rays. The spatial distribution of these stars is thus im
Externí odkaz:
http://arxiv.org/abs/1302.1223
Publikováno v:
Phys.Rev.Lett.103:031301,2009
Assuming Galactic positrons do not go far before annhilating, a difference between the observed 511 keV annihilation flux distribution and that of positron production, expected from beta-plus decay in Galactic iron nucleosynthesis, was evoked as evid
Externí odkaz:
http://arxiv.org/abs/0904.1025
Publikováno v:
Astrophys.J.698:350-379,2009
We consider positron propagation in the interstellar medium and show that the positrons from the beta-plus decay chains of the radioactive nuclei Ni-56, Ti-44, and Al-26, produced in Galactic supernovae, can fully account for all the features of the
Externí odkaz:
http://arxiv.org/abs/0711.3008
Publikováno v:
Astrophys.J. 611 (2004) L29-L32
The origin of the long-lived radioactive 26Al, which has been observed in the Galactic interstellar medium from its 1.809 MeV decay gamma-ray line emission, has been a persistent problem for over twenty years. Wolf-Rayet (WR) winds were thought to be
Externí odkaz:
http://arxiv.org/abs/astro-ph/0407172
Autor:
Rothschild, R. E., Lingenfelter, R. E.
Publikováno v:
Astrophys.J. 582 (2003) 257-261
Two long observations of Cas A supernova remnant were made by the \emph{Rossi X-ray Timing Explorer} in 1996 and 1997 to search for hard X-ray line emission at 67.9 and 78.4 keV from decay of $^{44}$Ti formed during the supernova event. Continuum flu
Externí odkaz:
http://arxiv.org/abs/astro-ph/0202043
Autor:
Kaplan, D. L., Kulkarni, S. R., van Kerkwijk, M. H., Rothschild, R. E., Lingenfelter, R. L., Marsden, D., Danner, R., Murakami, T.
Soft Gamma-ray Repeaters (SGRs) are among the most enigmatic sources known today. Exhibiting huge X- and Gamma-ray bursts and flares, as well as soft quiescent X-ray emission, their energy source remains a mystery. Just as mysterious are the Anomalou
Externí odkaz:
http://arxiv.org/abs/astro-ph/0103179
Pulsars associated with supernova remnants (SNRs) are valuable because they provide constraints on the mechanism(s) of pulsar spin-down. Here we discuss two SNR/pulsar associations in which the SNR age is much greater than the age of the pulsar obtai
Externí odkaz:
http://arxiv.org/abs/astro-ph/0102049
We discuss the highlights of our recent research, specifically the refractory vs. volatile interpretation of the rise of [O/Fe] with decreasing [Fe/H], and the issue of primary vs. secondary evolution of Be.
Comment: latex 2 pages, to be publish
Comment: latex 2 pages, to be publish
Externí odkaz:
http://arxiv.org/abs/astro-ph/0101432
Radio pulsars are thought to spin-down primarily due to torque from magnetic dipole radiation (MDR) emitted by the time-varying stellar magnetic field as the star rotates. This assumption yields a `characteristic age' for a pulsar which has generally
Externí odkaz:
http://arxiv.org/abs/astro-ph/0008300
Employing a Monte-Carlo based evolutionary code, we show that the delay of Fe deposition relative to O, due to the incorporation of supernova ejecta refractories in high velocity grains, can account for the rise of [O/Fe] with decreasing [Fe/H]. The
Externí odkaz:
http://arxiv.org/abs/astro-ph/0007273