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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

https://creativecommons.org/licenses/by/4.0/

Cobertura temática

Ciencias físicas

Tabla de contenidos

doi: 10.3847/1538-4357/ab1eb0

Relative Alignment between the Magnetic Field and Molecular Gas Structure in the Vela C Giant Molecular Cloud Using Low- and High-density Tracers

Laura M. Fissel; Peter A. R. Ade; Francesco E. Angilè; Peter Ashton; Steven J. Benton; Che-Yu Chen; Maria Cunningham; Mark J. Devlin; Bradley Dober; Rachel Friesen; Yasuo Fukui; Nicholas Galitzki; Natalie N. Gandilo; Alyssa Goodman; Claire-Elise Green; Paul Jones; Jeffrey Klein; Patrick King; Andrei L. Korotkov; Zhi-Yun Li; Vicki Lowe; Peter G. Martin; Tristan G. Matthews; Lorenzo Moncelsi; Fumitaka Nakamura; Calvin B. Netterfield; Amanda Newmark; Giles Novak; Enzo Pascale; Frédérick Poidevin; Fabio P. Santos; Giorgio Savini; Douglas Scott; Jamil A. Shariff; Juan D. Soler; Nicholas E. Thomas; Carole E. Tucker; Gregory S. Tucker; Derek Ward-Thompson; Catherine Zucker

Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.

Pp. 110

doi: 10.3847/1538-4357/ab1d67

An Initial Overview of the Extent and Structure of Recent Star Formation within the Serpens Molecular Cloud Using Gaia Data Release 2

Gregory J. Herczeg; Michael A. Kuhn; Xingyu Zhou; Jennifer Hatchell; Carlo F. Manara; Doug Johnstone; Michael Dunham; Anupam Bhardwaj; Jessy Jose; Zhen Yuan

Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.

Pp. 111

doi: 10.3847/1538-4357/ab1d64

Quasi-periodic Pulsations before and during a Solar Flare in AR 12242

Xingyao Chen; Yihua Yan; Baolin Tan; Jing Huang; Wei Wang; Linjie Chen; Yin Zhang; Chengming Tan; Donghao Liu; Satoshi Masuda

<jats:title>Abstract</jats:title> <jats:p>Quasi-periodic pulsations (QPPs) are frequently observed in solar flares, which may reveal some essential characteristics of both thermal and nonthermal energy releases. This work presents multi-wavelength imaging observations of an M8.7 flare in active region AR 12242 on 2014 December 17. We found that there were three different QPPs: UV QPPs with a period of about 4 minutes at 1600 Å images near the center of the active region lasting from the preflare phase to the impulsive phase; EUV QPPs with a period of about 3 minutes along the circular ribbon during the preflare phase; and radio QPPs with a period of about 2 minutes at frequencies of 1.2–2.0 GHz around the flaring source region during the impulsive phase. The observations include the radio images observed by the Mingantu Spectral Radioheliograph in China at frequencies of 1.2–2.0 GHz for the first time, microwave images by the Nobeyama Radioheliograph, UV and EUV images by AIA/<jats:italic>SDO</jats:italic>, and a magnetogram by HMI/<jats:italic>SDO</jats:italic>. We suggest that the 4 minute UV QPPs should be modulated by the sunspot oscillations, and the 3 minute EUV QPPs are closely related to the 2 minute radio QPPs for their source regions connected by a group of coronal loops. We propose that the intermittent magnetic reconnecting downward and upward plasmoids may be the possible trigger of both the preflare 3 minute EUV QPPs and the impulsive 2 minute radio QPPs. The other possible mechanism is LRC oscillation, which is associated with the current-carrying coronal loops. The latter mechanism implies that the existence of preflare QPPs may be a possible precursor to solar flares.</jats:p>

Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.

Pp. 78

Accedé al texto completo

doi: 10.3847/1538-4357/ab20ca

Orbital Migration of Interacting Stellar Mass Black Holes in Disks around Supermassive Black Holes

Amy Secunda; Jillian Bellovary; Mordecai-Mark Mac Low; K. E. Saavik Ford; Barry McKernan; Nathan W. C. Leigh; Wladimir Lyra; Zsolt Sándor

<jats:title>Abstract</jats:title> <jats:p>The merger rate of stellar-mass black hole binaries (sBHBs) inferred by the Advanced Laser Interferometer Gravitational-Wave Observatory (LIGO) suggests the need for an efficient source of sBHB formation. Active galactic nucleus (AGN) disks are a promising location for the formation of these sBHBs, as well as binaries of other compact objects, because of powerful torques exerted by the gas disk. These gas torques cause orbiting compact objects to migrate toward regions in the disk where inward and outward torques cancel, known as migration traps. We simulate the migration of stellar mass black holes in an example of a model AGN disk, using an augmented <jats:italic>N</jats:italic>-body code that includes analytic approximations to migration torques, stochastic gravitational forces exerted by turbulent density fluctuations in the disk, and inclination and eccentricity dampening produced by passages through the gas disk, in addition to the standard gravitational forces between objects. We find that sBHBs form rapidly in our model disk as stellar-mass black holes migrate toward the migration trap. These sBHBs are likely to subsequently merge on short timescales. The process continues, leading to the build-up of a population of over-massive stellar-mass black holes. The formation of sBHBs in AGN disks could contribute significantly to the sBHB merger rate inferred by LIGO.</jats:p>

Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.

Pp. 85

Accedé al texto completo

doi: 10.3847/1538-4357/ab1f6b

Turbulence and Particle Acceleration in Collisionless Magnetic Reconnection: Effects of Temperature Inhomogeneity across Pre-reconnection Current Sheet

San Lu; V. Angelopoulos; A. V. Artemyev; P. L. Pritchett; J. Liu; A. Runov; A. Tenerani; C. Shi; M. Velli

<jats:title>Abstract</jats:title> <jats:p>Magnetic reconnection is an important process in various collisionless plasma environments because it reconfigures the magnetic field and releases magnetic energy to accelerate charged particles. Its dynamics depend critically on the properties of the pre-reconnection current sheet. One property in particular, cross-sheet temperature inhomogeneity, which is ubiquitous throughout the heliosphere, has been shown to increase reconnection outflow speed, energy conversion efficiency, and secondary island formation rate using two-dimensional particle-in-cell simulations. Here we expand upon these findings, considering two cases with a long, thin current sheet, one with homogeneous temperature and one with inhomogeneous temperature across the current sheet. In the inhomogeneous temperature case, numerous secondary islands form continuously, which increases current sheet turbulence (well-developed cascade power spectra) at large wavenumbers. Current density, energy conversion, dissipation, and acceleration of high-energy particles are also enhanced relative to the homogenous temperature case. Our results suggest that inhomogeneous temperature profiles, which are realistic, need to be incorporated into studies of turbulence and particle acceleration in collisionless magnetic reconnection.</jats:p>

Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.

Pp. 109