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
A New Line-by-line General Circulation Model for Simulations of Diverse Planetary Atmospheres: Initial Validation and Application to the Exoplanet GJ 1132b
Feng Ding
; Robin D. Wordsworth
Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.
Pp. 117
Photochemical Hazes in Sub-Neptunian Atmospheres with a Focus on GJ 1214b
Panayotis Lavvas; Tommi Koskinen; Maria E. Steinrueck; Antonio García Muñoz; Adam P. Showman
Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.
Pp. 118
Retrieval of the Fluid Love Number k 2 in Exoplanetary Transit Curves
Hugo Hellard; Szilárd Csizmadia; Sebastiano Padovan; Heike Rauer; Juan Cabrera; Frank Sohl; Tilman Spohn; Doris Breuer
Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.
Pp. 119
Probing ISM Structure in Trumpler 14 and Carina I Using the Stratospheric Terahertz Observatory 2
Young Min Seo; Paul F. Goldsmith; Christopher K. Walker; David J. Hollenbach; Mark G. Wolfire; Craig A. Kulesa; Volker Tolls; Pietro N. Bernasconi; Ümit Kavak; Floris F. S. van der Tak; Russ Shipman; Jian Rong Gao; Alexander Tielens; Michael G. Burton; Harold Yorke; Erick Young; William L. Peters; Abram Young; Christopher Groppi; Kristina Davis; Jorge L. Pineda; William D. Langer; Jonathan H. Kawamura; Antony Stark; Gary Melnick; David Rebolledo; Graeme F. Wong; Shinji Horiuchi; Thomas B. Kuiper
Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.
Pp. 120
Spectral and Timing Analysis of the Accretion-powered Pulsar 4U 1626–67 Observed with Suzaku and NuSTAR
Wataru B. Iwakiri; Katja Pottschmidt; Sebastian Falkner; Paul B. Hemphill; Felix Fürst; Osamu Nishimura; Fritz-Walter Schwarm; Michael T. Wolff; Diana M. Marcu-Cheatham; Deepto Chakrabarty; John A. Tomsick; Colleen A. Wilson-Hodge; Matthias Bissinger Kühnel; Yukikatsu Terada; Teruaki Enoto; Jörn Wilms
Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.
Pp. 121
The Importance of Secondary Halos for Strong Lensing in Massive Galaxy Clusters across Redshift
Nan Li; Michael D. Gladders; Katrin Heitmann; Esteban M. Rangel; Hillary L. Child; Michael K. Florian; Lindsey E. Bleem; Salman Habib; Hal J. Finkel
Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.
Pp. 122
Benchmark for the Determination of the Positronium Formation Fraction in Interstellar Media
Daniel G. Cocks; Himanshu Chaudhary; Joshua R. Machacek
Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.
Pp. 123
On Geometrical Invariants of the Magnetic Field Gradient Tensor in Turbulent Space Plasmas: Scale Variability in the Inertial Range
Virgilio Quattrociocchi; Giuseppe Consolini; Maria Federica Marcucci; Massimo Materassi
Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.
Pp. 124
Gas and Dust Properties in the Chamaeleon Molecular Cloud Complex Based on the Optically Thick H i
Katsuhiro Hayashi; Ryuji Okamoto; Hiroaki Yamamoto; Takahiro Hayakawa; Kengo Tachihara; Yasuo Fukui
<jats:title>Abstract</jats:title> <jats:p>Gas and dust properties in the Chamaeleon molecular cloud complex have been investigated with emission lines from the atomic hydrogen (H <jats:sc>i</jats:sc>) and <jats:sup>12</jats:sup>CO molecules, dust optical depth at 353 GHz (<jats:italic>τ</jats:italic> <jats:sub>353</jats:sub>), and <jats:italic>J</jats:italic>-band infrared extinction (<jats:italic>A</jats:italic> <jats:sub> <jats:italic>J</jats:italic> </jats:sub>). We have found a scatter correlation between the H <jats:sc>i</jats:sc> integrated intensity (<jats:italic>W</jats:italic> <jats:sub>H <jats:sc>i</jats:sc> </jats:sub>) and <jats:italic>τ</jats:italic> <jats:sub>353</jats:sub> in the Chamaeleon region. The scattering has been examined in terms of a possible large optical depth in H <jats:sc>i</jats:sc> emission (<jats:italic>τ</jats:italic> <jats:sub>H <jats:sc>i</jats:sc> </jats:sub>) using a total column density (<jats:italic>N</jats:italic> <jats:sub>H</jats:sub>) model based on <jats:italic>τ</jats:italic> <jats:sub>353</jats:sub>. A nonlinear relation of <jats:italic>τ</jats:italic> <jats:sub>353</jats:sub> with the ∼1.2 power of <jats:italic>A</jats:italic> <jats:sub> <jats:italic>J</jats:italic> </jats:sub> has been found in opaque regions (<jats:italic>A</jats:italic> <jats:sub> <jats:italic>J</jats:italic> </jats:sub> ≳ 0.3 mag), which may indicate a dust evolution effect. If we apply this nonlinear relation to the <jats:italic>N</jats:italic> <jats:sub>H</jats:sub> model (i.e., <jats:italic>N</jats:italic> <jats:sub>H</jats:sub> ∝ <jats:inline-formula> <jats:tex-math> <?CDATA ${\tau }_{353}^{1/1.2}$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msubsup> <mml:mrow> <mml:mi>τ</mml:mi> </mml:mrow> <mml:mrow> <mml:mn>353</mml:mn> </mml:mrow> <mml:mrow> <mml:mn>1</mml:mn> <mml:mrow> <mml:mo stretchy="true">/</mml:mo> </mml:mrow> <mml:mn>1.2</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjab2051ieqn1.gif" xlink:type="simple" /> </jats:inline-formula>) allowing arbitrary <jats:italic>τ</jats:italic> <jats:sub>H <jats:sc>i</jats:sc> </jats:sub>, the model curve reproduces well the <jats:italic>W</jats:italic> <jats:sub>H <jats:sc>i</jats:sc> </jats:sub>–<jats:italic>τ</jats:italic> <jats:sub>353</jats:sub> scatter correlation, suggesting optically thick H <jats:sc>i</jats:sc> (<jats:italic>τ</jats:italic> <jats:sub>H <jats:sc>i</jats:sc> </jats:sub> ∼ 1.3) extended around the molecular clouds. Based on the correlations between the CO integrated intensity and the <jats:italic>N</jats:italic> <jats:sub>H</jats:sub> model, we have derived the CO-to-H<jats:sub>2</jats:sub> conversion factor (<jats:italic>X</jats:italic> <jats:sub>CO</jats:sub>) on ∼1.°5 scales (corresponding to ∼4 pc) and found spatial variations of <jats:italic>X</jats:italic> <jats:sub>CO</jats:sub> ∼ (0.5–3) × 10<jats:sup>20</jats:sup> cm<jats:sup>−2</jats:sup> K<jats:sup>−1</jats:sup> km<jats:sup>−1</jats:sup> s across the cloud complex, possibly depending on the radiation field inside or surrounding the molecular clouds. These gas properties found in the Chamaeleon region are discussed through a comparison with other local molecular cloud complexes.</jats:p>
Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.
Pp. 131
Radio Emission from Pulsars due to Relativistic Plasma
Tridib Roy; R. T. Gangadhara
<jats:title>Abstract</jats:title> <jats:p>Pulsar radio emission is not well understood because of a lack of knowledge about the emission geometry and the plasma process involved. We develop a mechanism for pulsar radio emission that takes into account the detailed viewing geometry of pulsars and the dipolar magnetic field configuration. Using a suitably chosen geometry and plasma parameters, we derive analytical expressions for the Stokes parameters of the radiation field in the frame centered on the neutron star. We have simulated pulse profiles based on our analytical formulation. It seems that we can explain the enhanced radiation and most of the diverse polarization properties of radio pulsars. We have estimated the brightness temperature, which seems to agree with the observations. The polarization angle predicted by the model is in good agreement with the rotating vector model.</jats:p>
Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.
Pp. 148