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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

Creative Commons Atribución No comercial No obras derivadas Compartir igual

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

Cobertura temática

Tabla de contenidos

Transport of Protostellar Cosmic Rays in Turbulent Dense Cores

Margot Fitz AxenORCID; Stella S. S. OffnerORCID; Brandt A. L. GachesORCID; Chris L. FryerORCID; Aimee Hungerford; Kedron SilsbeeORCID

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

Pp. 43

Detection of 7Be ii in the Classical Nova V5669 Sgr (Nova Sagittarii 2015 No.3)

Akira AraiORCID; Akito TajitsuORCID; Hideyo KawakitaORCID; Yoshiharu ShinnakaORCID

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

Pp. 44

Variations in Finite-difference Potential Fields

Ronald M. CaplanORCID; Cooper DownsORCID; Jon A. LinkerORCID; Zoran MikicORCID

<jats:title>Abstract</jats:title> <jats:p>The potential field (PF) solution of the solar corona is a vital modeling tool for a wide range of applications, including minimum energy estimates, coronal magnetic field modeling, and empirical solar wind solutions. Given its popularity, it is important to understand how choices made in computing a PF may influence key properties of the solution. Here we study PF solutions for the global coronal magnetic field on 2012 June 13, computed with our high-performance finite-difference code POT3D. Solutions are analyzed for their global properties and locally around NOAA AR 11504, using the net open flux, open-field boundaries, total magnetic energy, and magnetic structure as metrics. We explore how PF solutions depend on (1) the data source, type, and processing of the inner boundary conditions; (2) the choice of the outer boundary condition height and type; and (3) the numerical resolution and spatial scale of information at the lower boundary. We discuss the various qualitative and quantitative differences that naturally arise by using different maps as input, and we illustrate how coronal morphology and open flux depend most strongly on the outer boundary condition. We also show how large-scale morphologies and the open magnetic flux are remarkably insensitive to model resolution, while the surface mapping and embedded magnetic complexity vary considerably. This establishes important context for past, current, and future applications of the PF for coronal and solar wind modeling.</jats:p>

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

Pp. 44

The Core Mass Function across Galactic Environments. III. Massive Protoclusters

Theo J. O’NeillORCID; Giuliana CosentinoORCID; Jonathan C. TanORCID; Yu ChengORCID; Mengyao LiuORCID

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

Pp. 45

Longitudinally Resolved Spectral Retrieval (ReSpect) of WASP-43b

Patricio E. CubillosORCID; Dylan KeatingORCID; Nicolas B. CowanORCID; Johanna M. VosORCID; Ben BurninghamORCID; Marie YgoufORCID; Theodora KaralidiORCID; Yifan ZhouORCID; Eileen C. GonzalesORCID

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

Pp. 45

NOEMA Redshift Measurements of Extremely Bright Submillimeter Galaxies near the GOODS-N

Logan H. JonesORCID; Michael J. RosenthalORCID; Amy J. BargerORCID; Lennox L. CowieORCID

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

Pp. 46

ALMA Host Galaxy Observation of the Off-axis Gamma-Ray Burst XRF 020903

Jheng-Cyun Chen; Yuji UrataORCID; Kuiyun Huang

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

Pp. 46

GECKO Optical Follow-up Observation of Three Binary Black Hole Merger Events: GW190408_181802, GW190412, and GW190503_185404

Joonho KimORCID; Myungshin ImORCID; Gregory S. H. Paek; Chung-Uk LeeORCID; Seung-Lee KimORCID; Seo-Won ChangORCID; Changsu Choi; Sungyong HwangORCID; Wonseok Kang; Sophia Kim; Taewoo Kim; Hyung Mok Lee; Gu Lim; Jinguk Seo; Hyun-Il SungORCID

<jats:title>Abstract</jats:title> <jats:p>We present optical follow-up observation results of three binary black hole merger (BBH) events, GW190408_181802, GW190412, and GW190503_185404, which were detected by the Advanced LIGO and Virgo gravitational wave (GW) detectors. Electromagnetic (EM) counterparts are generally not expected for BBH merger events. However, some theoretical models suggest that EM counterparts of BBH can possibly arise in special environments, prompting motivation to search for EM counterparts for such events. We observed high-credibility regions of the sky for the three BBH merger events with telescopes of the Gravitational-wave EM Counterpart Korean Observatory (GECKO), including the KMTNet. Our observation started as soon as 100 minutes after the GW event alerts and covered 29–63 deg<jats:sup>2</jats:sup> for each event with a depth of ∼22.5 mag in the <jats:italic>R </jats:italic>band within hours of observation. No plausible EM counterparts were found for these events, but based on there being no detection of the GW190503_185404 event, for which we covered the 69% credibility region, we place the BBH merger EM counterpart signal to be <jats:italic>M</jats:italic> <jats:sub> <jats:italic>g</jats:italic> </jats:sub> &gt; − 18.0 AB mag within about one day of the GW event. The comparison of our detection limits with light curves of several kilonova models suggests that a kilonova event could have been identified within hours of the GW alert with GECKO observations if the compact merger happened at &lt;400 Mpc and the localization accuracy was on the order of 50 deg<jats:sup>2</jats:sup>. Our result shows great promise for the GECKO facilities to find EM counterparts within a few hours from GW detection in future GW observation runs.</jats:p>

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

Pp. 47

Star Formation Rate Function at z ∼ 4.5: An Analysis from Rest UV to Optical

Yoshihisa AsadaORCID; Kouji OhtaORCID; Fumiya MaedaORCID

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

Pp. 47

Accretion onto Stars in the Disks of Active Galactic Nuclei

Alexander J. DittmannORCID; Matteo CantielloORCID; Adam S. JermynORCID

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

Pp. 48