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
An 86 GHz Search for Pulsars in the Galactic Center with the Atacama Large Millimeter / submillimeter Array
Kuo Liu
; Gregory Desvignes; Ralph P. Eatough; Ramesh Karuppusamy; Michael Kramer; Pablo Torne; Robert Wharton; Shami Chatterjee; James M. Cordes; Geoffrey B. Crew; Ciriaco Goddi; Scott M. Ransom; Helge Rottmann; Federico Abbate; Geoffrey C. Bower; Christiaan D. Brinkerink; Heino Falcke; Aristeidis Noutsos; Antonio Hernández-Gómez; Wu Jiang; Michael D. Johnson; Ru-Sen Lu; Yurii Pidopryhora; Luciano Rezzolla; Lijing Shao; Zhiqiang Shen; Norbert Wex
Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.
Pp. 30
Magnetohydrodynamic Winds Driven by the Line Force from the Standard Thin Disk around Supermassive Black Holes. I. The Case of Weak Magnetic Field
Xiao-Hong Yang; Kamarjan Ablimit; Qi-Xiu Li
<jats:title>Abstract</jats:title> <jats:p>Absorption lines with high blueshifted velocities are frequently found in the ultraviolet (UV) and X-ray spectra of luminous active galactic nuclei (AGNs). This implies that high-velocity winds/outflows are common in AGNs. In order to study the formation of high-velocity winds, especially ultrafast outflows (UFOs), we perform two-dimensional magnetohydrodynamic (MHD) simulations. Initially, a magnetic field is set to be weaker than the gas pressure at the disk surface. In our simulations, line force operates on the region like filaments because the X-ray radiation from corona is shielded by dense gas in the inner region at some angle. The location of filaments changes with time and then the line-driven winds are exposed to X-rays and become highly ionized. The line force at the UV bands does not directly drive the highly ionized winds. In the sense of time average, the properties of high-velocity winds meet the formation condition of UFOs. Compared with line force, the function of magnetic field is negligible in directly driving winds. In the MHD model, the region around the rotational axis becomes magnetic-pressure dominated, which prevents gases from spreading to higher latitudes and then enhances the gas column density at middle and low latitudes (20°–70°). Higher column density is helpful to shield X-ray photons, which causes the line force to be more effective in the MHD model than in the hydrodynamic model. Higher-velocity winds with a broader opening angle are produced in the MHD model.</jats:p>
Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.
Pp. 31
Parameterizing the Outflow from a Central Black Hole in Dwarf Spheroidal Galaxies: A 3D Hydrodynamic Simulation
Gustavo A. Lanfranchi; Roberto Hazenfratz; Anderson Caproni; Joseph Silk
Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.
Pp. 32
The Influence of the Secular Perturbation of an Intermediate-mass Companion. II. Ejection of Hypervelocity Stars from the Galactic Center
Xiaochen Zheng; Douglas N. C. Lin; Shude Mao
Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.
Pp. 33
High-resolution Laboratory Measurements of K-shell X-Ray Line Polarization and Excitation Cross Sections in Helium-like S XV Ions
Chintan Shah; Natalie Hell; Antonia Hubbard; Ming Feng Gu; Michael J. MacDonald; Megan E. Eckart; Richard L. Kelley; Caroline A. Kilbourne; Maurice A. Leutenegger; F. Scott Porter; Gregory V. Brown
Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.
Pp. 34
Multiepoch Optical Images of IRC+10216 Tell about the Central Star and the Adjacent Environment
Hyosun Kim; Ho-Gyu Lee; Youichi Ohyama; Ji Hoon Kim; Peter Scicluna; You-Hua Chu; Nicolas Mauron; Toshiya Ueta
Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.
Pp. 35
Subaru High-z Exploration of Low-luminosity Quasars (SHELLQs). XIII. Large-scale Feedback and Star Formation in a Low-luminosity Quasar at z = 7.07 on the Local Black Hole to Host Mass Relation
Takuma Izumi; Yoshiki Matsuoka; Seiji Fujimoto; Masafusa Onoue; Michael A. Strauss; Hideki Umehata; Masatoshi Imanishi; Kotaro Kohno; Toshihiro Kawaguchi; Taiki Kawamuro; Shunsuke Baba; Tohru Nagao; Yoshiki Toba; Kohei Inayoshi; John D. Silverman; Akio K. Inoue; Soh Ikarashi; Kazushi Iwasawa; Nobunari Kashikawa; Takuya Hashimoto; Kouichiro Nakanishi; Yoshihiro Ueda; Malte Schramm; Chien-Hsiu Lee; Hyewon Suh
Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.
Pp. 36
The Search for Binary Supermassive Black Holes among Quasars with Offset Broad Lines Using the Very Long Baseline Array
Peter Breiding; Sarah Burke-Spolaor; Michael Eracleous; Tamara Bogdanović; T. Joseph W. Lazio; Jessie Runnoe; Steinn Sigurdsson
<jats:title>Abstract</jats:title> <jats:p>In several previous studies, quasars exhibiting broad emission lines with ≳1000 km s<jats:sup>−1</jats:sup> velocity offsets with respect to the host galaxy rest frame have been discovered. One leading hypothesis for the origin of these velocity-offset broad lines is the dynamics of a binary supermassive black hole (SMBH). We present high-resolution radio imaging of 34 quasars showing these velocity-offset broad lines with the Very Long Baseline Array (VLBA), aiming to find evidence for the putative binary SMBHs (such as dual radio cores), and testing the competing physical models. We detect exactly half of the target sample from our VLBA imaging, after implementing a 5<jats:italic>σ</jats:italic> detection limit. While we do not resolve double radio sources in any of the targets, we obtain limits on the instantaneous projected separations of a radio-emitting binary for all of the detected sources under the assumption that a binary still exists within our VLBA angular resolution limits. We also assess the likelihood that a radio-emitting companion SMBH exists outside of our angular resolution limits, but its radio luminosity is too weak to produce a detectable signal in the VLBA data. Additionally, we compare the precise sky positions afforded by these data to optical positions from both the SDSS and Gaia DR2 source catalogs. We find projected radio/optical separations on the order of ∼10 pc for three quasars. Finally, we explore how future multi-wavelength campaigns with optical, radio, and X-ray observatories can help discriminate further between the competing physical models.</jats:p>
Palabras clave: Industrial and Manufacturing Engineering; Materials Science (miscellaneous); Business and International Management.
Pp. 37
How to Identify Exoplanet Surfaces Using Atmospheric Trace Species in Hydrogen-dominated Atmospheres
Xinting Yu; Julianne I. Moses; Jonathan J. Fortney; Xi Zhang
Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.
Pp. 38
Modeling a Coronal Mass Ejection from an Extended Filament Channel. I. Eruption and Early Evolution
Benjamin J. Lynch; Erika Palmerio; C. Richard DeVore; Maria D. Kazachenko; Joel T. Dahlin; Jens Pomoell; Emilia K. J. Kilpua
<jats:title>Abstract</jats:title> <jats:p>We present observations and modeling of the magnetic field configuration, morphology, and dynamics of a large-scale, high-latitude filament eruption observed by the Solar Dynamics Observatory. We analyze the 2015 July 9–10 filament eruption and the evolution of the resulting coronal mass ejection (CME) through the solar corona. The slow streamer-blowout CME leaves behind an elongated post-eruption arcade above the extended polarity inversion line that is only poorly visible in extreme ultraviolet (EUV) disk observations and does not resemble a typical bright flare-loop system. Magnetohydrodynamic (MHD) simulation results from our data-inspired modeling of this eruption compare favorably with the EUV and white-light coronagraph observations. We estimate the reconnection flux from the simulation’s flare-arcade growth and examine the magnetic-field orientation and evolution of the erupting prominence, highlighting the transition from an erupting sheared-arcade filament channel into a streamer-blowout flux-rope CME. Our results represent the first numerical modeling of a global-scale filament eruption where multiple ambiguous and complex observational signatures in EUV and white light can be fully understood and explained with the MHD simulation. In this context, our findings also suggest that the so-called stealth CME classification, as a driver of unexpected or “problem” geomagnetic storms, belongs more to a continuum of observable/nonobservable signatures than to separate or distinct eruption processes.</jats:p>
Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.
Pp. 39