Annales Geophysicae Journal Impact Factor & Information

Publisher: European Geophysical Society, European Geosciences Union

Journal description

Prior to 2001 this journal was published by Springer. Annales Geophysicae (ANGEO) is an international, multi- and inter- disciplinary scientific journal for the publication of original articles and of short communications (Letters) for the sciences of the Sun-Earth system, including the science of Space Weather, the Solar-Terrestrial plasma physics, and the Earth's atmosphere and oceans.

Current impact factor: 1.68

Impact Factor Rankings

2015 Impact Factor Available summer 2015
2013 / 2014 Impact Factor 1.676
2012 Impact Factor 1.518
2011 Impact Factor 1.842
2010 Impact Factor 1.62
2009 Impact Factor 1.648
2008 Impact Factor 1.66
2007 Impact Factor 1.427
2006 Impact Factor 1.293
2005 Impact Factor 1.45
2004 Impact Factor 1.61
2003 Impact Factor 1.031
2002 Impact Factor 1.189
2001 Impact Factor 1.199
2000 Impact Factor 1.76
1999 Impact Factor 1.727
1998 Impact Factor 1.423
1997 Impact Factor 1.245

Impact factor over time

Impact factor

Additional details

5-year impact 1.63
Cited half-life 7.30
Immediacy index 0.26
Eigenfactor 0.02
Article influence 0.77
Website Annales Geophysicae (1988) website
Other titles Annales geophysicae (Montrouge, France: 1988: Online), Annales geophysicae
ISSN 1432-0576
OCLC 41977993
Material type Document, Periodical, Internet resource
Document type Internet Resource, Computer File, Journal / Magazine / Newspaper

Publisher details

European Geosciences Union

  • Pre-print
    • Author can archive a pre-print version
  • Post-print
    • Author can archive a post-print version
  • Conditions
    • Authors retain copyright
    • Creative Commons Attribution License 3.0
    • Eligible UK authors may deposit in OpenDepot
    • Publisher's version/PDF may be used
    • All titles are open access journals
  • Classification
    ​ green

Publications in this journal

  • [Show abstract] [Hide abstract]
    ABSTRACT: We analyze the results from numerical simulations of the magnetic field, the electric field and the plasma particle dynamics at the inner geospace under the effect of solar storms and magnetospheric substorms. An orbit-following model solves for the full-particle motion, employing a dynamic, solar wind-driven geomagnetic field with a description of the electric field due to plasma convection and magnetic induction, all cast in a form suitable for implementation in computer codes. The kinematic data from the test-particle simulations is statistically analyzed over the initial plasma state, and an estimation of the charged particle fluxes from different populations and of the ensemble-averaged Dst index (based on the ring and tail current contributions) is provided. The present model may serve as the final link in a Sun-to-Earth modeling chain of major solar eruptions, providing an estimation of the inner geospace response.
    Annales Geophysicae 07/2015;
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    ABSTRACT: The interval of geomagnetic storms of 7–17 March 2012 was selected at the Climate and Weather of the Sun-Earth System (CAWSES) II Workshop for group study of space weather effects during the ascending phase of solar cycle 24 (Tsurutani et al., 2014). The high-latitude ionospheric response to a series of storms is studied using arrays of GPS receivers, HF radars, ionosondes, riometers, magnetometers, and auroral imagers focusing on GPS phase scintillation. Four geomagnetic storms showed varied responses to solar wind conditions characterized by the interplanetary magnetic field (IMF) and solar wind dynamic pressure. As a function of magnetic latitude and magnetic local time, regions of enhanced scintillation are identified in the context of coupling processes between the solar wind and the magnetosphere–ionosphere system. Large southward IMF and high solar wind dynamic pressure resulted in the strongest scintillation in the nightside auroral oval. Scintillation occurrence was correlated with ground magnetic field perturbations and riometer absorption enhancements, and collocated with mapped auroral emission. During periods of southward IMF, scintillation was also collocated with ionospheric convection in the expanded dawn and dusk cells, with the antisunward convection in the polar cap and with a tongue of ionization fractured into patches. In contrast, large northward IMF combined with a strong solar wind dynamic pressure pulse was followed by scintillation caused by transpolar arcs in the polar cap.
    Annales Geophysicae 06/2015; 33(6):637-656. DOI:10.5194/angeo-33-637-2015
  • [Show abstract] [Hide abstract]
    ABSTRACT: During the ascending phase of solar cycle 24, a series of interplanetary coronal mass ejections (ICMEs) in the period 7–17 March 2012 caused geomagnetic storms that strongly affected high-latitude ionosphere in the Northern and Southern Hemisphere. GPS phase scintillation was observed at northern and southern high latitudes by arrays of GPS ionospheric scintillation and TEC monitors (GISTMs) and geodetic-quality GPS receivers sampling at 1 Hz. Mapped as a function of magnetic latitude and magnetic local time (MLT), the scintillation was observed in the ionospheric cusp, the tongue of ionization fragmented into patches, sun-aligned arcs in the polar cap, and nightside auroral oval and subauroral latitudes. Complementing a companion paper (Prikryl et al., 2015a) that focuses on the high-latitude ionospheric response to variable solar wind in the North American sector, interhemispheric comparison reveals commonalities as well as differences and asymmetries between the northern and southern high latitudes, as a consequence of the coupling between the solar wind and magnetosphere. The interhemispheric asymmetries are caused by the dawn–dusk component of the interplanetary magnetic field controlling the MLT of the cusp entry of the storm-enhanced density plasma into the polar cap and the orientation relative to the noon–midnight meridian of the tongue of ionization.
    Annales Geophysicae 06/2015; 33(6):657-670. DOI:10.5194/angeo-33-657-2015
  • [Show abstract] [Hide abstract]
    ABSTRACT: Ionospheric blobs are localized plasma density enhancements, which are mainly produced by the transportation process of plasma. To understand the deformation process of a blob, observations of plasma parameters with good spatial–temporal resolution are desirable. Thus, we conducted the European Incoherent Scatter radar observations with high-speed meridional scans (60–80 s) during October and December 2013, and observed the temporal evolution of a blob during a substorm on 4 December 2013. This paper is the first report of direct observations of blob deformation during a substorm. The blob deformation arose from an enhanced plasma flow shear during the substorm expansion phase, and then the blob split into two smaller-scale blobs, whose scale sizes were more than ~100 km in latitude. Our analysis indicates that the Kelvin–Helmholtz instability and dissociative recombination could have deformed the blob structure.
    Annales Geophysicae 05/2015; 33(5):525-530. DOI:10.5194/angeo-33-525-2015
  • Annales Geophysicae 01/2015; 33(6):687-695. DOI:10.5194/angeo-33-687-2015
  • Annales Geophysicae 01/2015; 33(6):703-709. DOI:10.5194/angeo-33-703-2015
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    ABSTRACT: A significant enhancement of radiation doses is expected for aircrews during ground-level enhancement (GLE) events, while the possible radiation hazard remains an open question during non-GLE solar energetic particle (SEP) events. Using a new air-shower simulation driven by the proton flux data obtained from GOES satellites, we show the possibility of significant enhancement of the effective dose rate of up to 4.5 mu Sv h(-1) at a conventional flight altitude of 12 km during the largest SEP event that did not cause a GLE. As a result, a new GOES-driven model is proposed to give an estimate of the contribution from the isotropic component of the radiation dose in the stratosphere during non-GLE SEP events.
    Annales Geophysicae 01/2015; 33(1):75-78. DOI:10.5194/angeo-33-75-2015
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    ABSTRACT: The inter-annual variations in wave spectrum are examined based on the wave data measured at 9m water depth off the central west coast of India from 2009 to 2012 using a wave rider buoy. The temporal variation of the spectral energy density over a calendar year indicates similar variation in all the four years studied. The inter-annual variations in wave spectrum are observed in all months with larger variations during January to February, May and October to November due to the changes in wind-sea. The seasonal average wave spectrum during the monsoon (June-September) is single-peaked and the swell component is high in 2011 compared to other years. The annual averaged wave spectrum had higher peak energy during 2011 due to the higher spectral energy present during the monsoon period. During the non-monsoon period, two peaks are predominantly observed in the wave spectra; with the average peak at 0.07 Hz corresponding to the swells from the Indian Ocean and another at 0.17 Hz due to the local wind field.
    Annales Geophysicae 01/2015; 33(2):159-167. DOI:10.5194/angeo-33-159-2015
  • Annales Geophysicae 01/2015; 33(3):413-426. DOI:10.5194/angeo-33-413-2015