Catálogo de publicaciones - revistas
Título de Acceso Abierto
The Astrophysical Journal (ApJ)
Resumen/Descripción – provisto por la editorial en inglés
The Astrophysical Journal is an open access journal devoted to recent developments, discoveries, and theories in astronomy and astrophysics. Publications in ApJ constitute significant new research that is directly relevant to astrophysical applications, whether based on observational results or on theoretical insights or modeling.Palabras clave – provistas por la editorial
astronomy; astrophysics
Disponibilidad
| Institución detectada | Período | Navegá | Descargá | Solicitá |
|---|---|---|---|---|
| No detectada | desde jul. 1995 / hasta dic. 2023 | IOPScience |
Información
Tipo de recurso:
revistas
ISSN impreso
0004-637X
ISSN electrónico
1538-4357
Editor responsable
American Astronomical Society (AAS)
Idiomas de la publicación
- inglés
País de edición
Reino Unido
Información sobre licencias CC
Cobertura temática
Tabla de contenidos
The Sun’s Magnetic (Hale) Cycle and 27 Day Recurrences in the aa Geomagnetic Index
S. C. Chapman
; S. W. McIntosh; R. J. Leamon; N. W. Watkins
Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.
Pp. 54
Efficiencies of Magnetic Field Amplification and Electron Acceleration in Young Supernova Remnants: Global Averages and Kepler’s Supernova Remnant
Stephen P. Reynolds; Brian J. Williams; Kazimierz J. Borkowski; Knox S. Long
Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.
Pp. 55
Back to Quiescence: Postoutburst Evolution of the Pulsar J1119–6127 and Its Wind Nebula
Harsha Blumer; Samar Safi-Harb; Alice Borghese; Jonatan Martín; Maura A. McLaughlin; Diego F. Torres; George Younes
Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.
Pp. 56
Probing Polarization and the Role of Magnetic Fields in Cloud Destruction in the Keyhole Nebula
Young Min Seo; C. Darren Dowell; Paul F. Goldsmith; Jorge L. Pineda; Liton Majumdar
Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.
Pp. 57
Future Constraints on the Reionization History and the Ionizing Sources from Gamma-Ray Burst Afterglows
Adam Lidz; Tzu-Ching Chang; Lluís Mas-Ribas; Guochao Sun
Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.
Pp. 58
Iron and Nickel Isotopes in IID and IVB Iron Meteorites: Evidence for Admixture of an SN II Component and Implications for the Initial Abundance of 60Fe
David L. Cook; Bradley S. Meyer; Maria Schönbächler
<jats:title>Abstract</jats:title> <jats:p>We measured Fe and Ni isotopes in 13 iron meteorites from magmatic groups <jats:sc>II</jats:sc>D and <jats:sc>IV</jats:sc>B. Resolvable deficits (≈−0.14) are observed in <jats:italic>ε</jats:italic> <jats:sup>60</jats:sup>Ni in both groups. Small deficits (≈−0.08) are also evident in <jats:italic>ε</jats:italic> <jats:sup>56</jats:sup>Fe but not in the most neutron-rich isotope of Fe (<jats:sup>58</jats:sup>Fe). Relative to terrestrial material, the observed <jats:italic>ε</jats:italic> <jats:sup>i</jats:sup>Fe values are consistent with the presence of a small excesses of material in the parent bodies of <jats:sc>II</jats:sc>D and <jats:sc>IV</jats:sc>B irons that was produced in a type <jats:sc>II</jats:sc> supernova. The <jats:italic>ε</jats:italic> <jats:sup>60</jats:sup>Ni and <jats:italic>ε</jats:italic> <jats:sup>56</jats:sup>Fe values are uncorrelated in both groups. This is consistent with a nucleosynthetic origin of the <jats:italic>ε</jats:italic> <jats:sup>56</jats:sup>Fe deficits, whereas the <jats:italic>ε</jats:italic> <jats:sup>60</jats:sup>Ni deficits are best explained as radiogenic in nature due to the former presence of live <jats:sup>60</jats:sup>Fe (<jats:italic>t</jats:italic> <jats:sub>1/2</jats:sub> = 2.62 Ma) in the early solar system. The <jats:sup>60</jats:sup>Ni deficits correspond to <jats:sup>60</jats:sup>Fe/<jats:sup>56</jats:sup>Fe ratios of ≈3 × 10<jats:sup>−7</jats:sup> at the time of core formation on the <jats:sc>II</jats:sc>D and <jats:sc>IV</jats:sc>B parent bodies. These data, in conjunction with previously published <jats:sup>182</jats:sup>Hf–<jats:sup>182</jats:sup>W core formation ages, are used to estimate a solar system initial <jats:sup>60</jats:sup>Fe/<jats:sup>56</jats:sup>Fe = (6.4 ± 2.0) × 10<jats:sup>−7</jats:sup> for the formation region of carbonaceous chondrites.</jats:p>
Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.
Pp. 59
Evolution of High-redshift Quasar Hosts and Promotion of Massive Black Hole Seed Formation
Wenxiu Li; Kohei Inayoshi; Yu Qiu
Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.
Pp. 60
A Magnetic Disk-outflow Model for Changing Look Active Galactic Nuclei
Junjie Feng; Xinwu Cao; Jia-wen Li; Wei-Min Gu
Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.
Pp. 61
Origin of Spectral Hardening of Secondary Cosmic-Ray Nuclei
Norita Kawanaka; Shiu-Hang Lee
Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.
Pp. 61
A Simulation of Radius-frequency Mapping for PSR J1848-0123 with an Inverse Compton Scattering Model
L. H. Shang; X. Xu; S. J. Dang; Q. J. Zhi; J. T. Bai; R. H. Zhu; Q. W. Lin; H. Yang
<jats:title>Abstract</jats:title> <jats:p>The radio radiation mechanism is one of the open questions for pulsars. Multiband observations are very helpful to constrain pulsar radiation models. We observed PSR J1848-0123 at the 5 GHz band with the Shanghai Tianma 65 m radio telescope (TMRT). The 5 GHz observation together with the European Pulsar Network (EPN) and CSIRO ATNF Data Archives databases provides a broadband evolution property of the pulse profiles for this pulsar. We reprocessed these data sets to obtain the multiband pulse profiles. It was found that the pulse profile of PSR J1848-0123 narrows with increasing emission frequency. We separated the emission components of each pulse profile with a multi-Gaussian fitting method, and then calculated the beaming angle and emission radius of each component with the basic radiation geometry of pulsar. With the calculated beam angles and radiation radii, we simulated the radius-frequency mapping of this pulsar with an inverse Compton scatting model (ICS). It was found that the observed radio radiation could be generated in the core gap region above the polar cap of the pulsar. The beaming angle and emission radius versus frequency for PSR J1848-0123 can be explained well with the ICS model.</jats:p>
Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.
Pp. 62