The Astrophysical Journal (ASTROPHYS J)

Publisher: American Astronomical Society; University of Chicago, American Astronomical Society

Journal description

The Astrophysical Journal is the foremost research journal in the world devoted to recent developments, discoveries, and theories in astronomy and astrophysics. Many of the classic discoveries of the twentieth century have first been reported in the Journal, which has also presented much of the important recent work on quasars, pulsars, neutron stars, black holes, solar and stellar magnetic fields, X-rays, and interstellar matter. The Astrophysical Journal Letters ( is Part 2 of The Astrophysical Journal. Letters articles are published first as unpaginated papers on University of Chicago Press's Rapid Release website, then moved to a complete electronic issue, and finally are published in print with Part 1 on the 1st, 10th, and 20th of every month.

Current impact factor: 5.99

Impact Factor Rankings

2016 Impact Factor Available summer 2017
2014 / 2015 Impact Factor 5.993
2013 Impact Factor 6.28
2012 Impact Factor 6.733
2011 Impact Factor 6.024
2010 Impact Factor 7.436
2009 Impact Factor 7.364
2008 Impact Factor 6.331
2007 Impact Factor 6.405
2006 Impact Factor 6.119
2005 Impact Factor 6.308
2004 Impact Factor 6.237
2003 Impact Factor 6.604
2002 Impact Factor 6.187
2001 Impact Factor 5.921
2000 Impact Factor 2.822
1999 Impact Factor 2.543
1998 Impact Factor 1.953
1997 Impact Factor 2.948
1996 Impact Factor 3.232
1995 Impact Factor 3.484
1994 Impact Factor 3.544
1993 Impact Factor 3.387
1992 Impact Factor 2.931

Impact factor over time

Impact factor

Additional details

5-year impact 5.64
Cited half-life 7.60
Immediacy index 1.74
Eigenfactor 0.52
Article influence 2.39
Website Astrophysical Journal, The website
Other titles The Astrophysical journal, ApJ
ISSN 0004-637X
OCLC 1518501
Material type Periodical, Internet resource
Document type Journal / Magazine / Newspaper, Internet Resource

Publisher details

American Astronomical Society

  • Pre-print
    • Author can archive a pre-print version
  • Post-print
    • Author can archive a post-print version
  • Conditions
    • On any website or open access repository
    • Publisher copyright and source must be acknowledged
    • Must link to publisher version
    • Publisher's version/PDF may be used
  • Classification

Publications in this journal

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    ABSTRACT: In recent years, the analysis of absorption lines in quasi-stellar object (QSO) spectra, using the many-multiplet (MM) method, has provided evidence for space–time variations in the fine-structure constant, α. Future studies aim to reduce systematic errors in these measurements by considering a greater number of transitions, but this is only possible for lines where high-precision laboratory standards exist. Two transitions of high importance for future MM analyses, but which currently lack accurately measured wavelengths, are the Ti ii transitions observed at 1910 Å. We report accurate measurements of these transitions by high-resolution Fourier transform spectroscopy, giving line wavenumbers of (52,329.889 ± 0.001) cm −1 and (52,339.240 ± 0.001) cm −1 . Lines from other important Ti ii, Mg i, Mg ii, and Zn ii transitions were measured simultaneously, minimizing their relative wavenumber uncertainties, and permitting the newly measured 1910 Å Ti ii line wavenumbers to be linked directly to lines from other studies.
    Preview · Article · Jul 2016 · The Astrophysical Journal
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    ABSTRACT: We consider interactions between protons and Alfvén/ion-cyclotron (A/IC) waves in collisionless low-β plasmas in which the proton distribution function f is strongly modified by wave pitch-angle scattering. If the angle θ between the wave vector and background magnetic field is zero for all the waves, then strong scattering causes f to become approximately constant on surfaces of constant η, where η v 2⊥ + 1.5 v 2/3A|v ∥|4/3. Here, v ⊥ and v ∥ are the velocity components perpendicular and parallel to the background magnetic field, and v A is the Alfvén speed. If f = f(η), then A/IC waves with θ = 0 are neither damped nor amplified by resonant interactions with protons. In this paper, we argue that if some mechanism generates high-frequency A/IC waves with a range of θ values, then wave-particle interactions initially cause the proton distribution function to become so anisotropic that the plasma becomes unstable to the growth of waves with θ = 0. The resulting amplification of θ = 0 waves leads to an angular distribution of A/IC waves that is sharply peaked around θ = 0 at the large wavenumbers at which A/IC waves resonate with protons. Scattering by this angular distribution of A/IC waves subsequently causes f to become approximately constant along surfaces of constant η, which in turn causes oblique A/IC waves to be damped by protons. We calculate the proton and electron contributions to the damping rate analytically, assuming Maxwellian electrons and f = f(η). Because the plasma does not relax to a state in which proton damping of oblique A/IC waves ceases, oblique A/IC waves can be significantly more effective at heating protons than A/IC waves with θ = 0.
    Preview · Article · May 2016 · The Astrophysical Journal
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    ABSTRACT: The cross-power spectrum is a quadratic estimator between two maps that can provide unbiased estimate of the underlying power spectrum of the correlated signals, which is therefore used for extracting the power spectrum in the Wilkinson Microwave Anisotropy Probe (WMAP) data. In this paper, we discuss the limit of the cross-power spectrum and derive the residual from the uncorrelated signal, which is the source of error in power spectrum extraction. We employ the estimator to extract window functions by crossing pairs of extragalactic point sources. We demonstrate its usefulness in WMAP difference assembly maps where the window functions are measured via Jupiter and then extract the window functions of the five WMAP frequency band maps.
    Preview · Article · Apr 2016 · The Astrophysical Journal
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    ABSTRACT: With the development of one-dimensional stellar evolution codes including rotation and the increasing number of observational data for stars of various evolutionary stages, it becomes more and more possible to follow the evolution of the rotation profile and angular momentum distribution in stars. In this context, understanding the interplay between rotation and convection in the very extended envelopes of giant stars is very important considering that all low-and intermediate-mass stars become red giants after the central hydrogen burning phase. In this paper, we analyze the interplay between rotation and convection in the envelope of red giant stars using three-dimensional numerical experiments. We make use of the Anelastic Spherical Harmonics code to simulate the inner 50% of the envelope of a low-mass star on the red giant branch. We discuss the organization and dynamics of convection, and put a special emphasis on the distribution of angular momentum in such a rotating extended envelope. To do so, we explore two directions of the parameter space, namely, the bulk rotation rate and the Reynolds number with a series of four simulations. We find that turbulent convection in red giant stars is dynamically rich, and that it is particularly sensitive to the rotation rate of the star. Reynolds stresses and meridional circulation establish various differential rotation profiles (either cylindrical or shellular) depending on the convective Rossby number of the simulations, but they all agree that the radial shear is large. Temperature fluctuations are found to be large and in the slowly rotating cases, a dominant = 1 temperature dipole influences the convective motions. Both baroclinic effects and turbulent advection are strong in all cases and mostly oppose one another.
    Preview · Article · Mar 2016 · The Astrophysical Journal
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    ABSTRACT: White-light observations of interplanetary disturbances have been dominated by interplanetary coronal mass ejections (ICMEs). This is because the other type of disturbance, the corotating interaction region (CIR), has proved difficult to detect using white-light imagers. Recently, a number of papers have appeared presenting CIR observations using the Solar Terrestrial Relations Observatory (STEREO) Heliospheric Imagers (HIs), but have mostly only focused on a single spacecraft and imager. In this paper, we present observations of a single CIR that was observed by all three current white-light heliospheric imagers (SMEI and both STEREO HIs), as well as the in situ instruments on both STEREO satellites and ACE. We begin with a discussion of the geometry of the CIR structure, and show how the apparent leading edge structure is expected to change as it corotates relative to the observer. We use these calculations to predict elongation–time profiles for CIRs of different speeds for each of the imagers, and also to predict the arrival times at the in situ instruments. We show that although all three measured different parts, they combine to produce a self-consistent picture of the CIR. Finally, we offer some thoughts on why CIRs have proved so difficult to detect in white-light heliospheric images.
    Preview · Article · Mar 2016 · The Astrophysical Journal