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Solar Coronal Jets: Observations, Theory, and Modeling

Space Science Reviews volume 201, pages 1–53 (2016)Cite this article

Abstract

Coronal jets represent important manifestations of ubiquitous solar transients, which may be the source of significant mass and energy input to the upper solar atmosphere and the solar wind. While the energy involved in a jet-like event is smaller than that of “nominal” solar flares and coronal mass ejections (CMEs), jets share many common properties with these phenomena, in particular, the explosive magnetically driven dynamics. Studies of jets could, therefore, provide critical insight for understanding the larger, more complex drivers of the solar activity. On the other side of the size-spectrum, the study of jets could also supply important clues on the physics of transients close or at the limit of the current spatial resolution such as spicules. Furthermore, jet phenomena may hint to basic process for heating the corona and accelerating the solar wind; consequently their study gives us the opportunity to attack a broad range of solar-heliospheric problems.

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Notes

  1. A typo in paragraph 2 of §5 of Moore et al. (2013) says “all 29 blow-out X-ray jets displayed a cool component.” This instead should read: “29 out of 32 blow-out X-ray jets displayed a cool component.” This typo does not affect the general discussion and conclusions of that paper.

  2. See http://solar.bnsc.rl.ac.uk/software/uguide/NIS_PSF/.

Abbreviations

AIA:

Atmospheric Imaging Assembly (Lemen et al. 2012)

AR(s):

Active region(s)

AU:

Astronomical unit

BP(s):

Bright point(s)

CBP(s):

Coronal bright point(s)

CDS:

Coronal Diagnostic Spectrometer (Harrison et al. 1995)

CH(s):

Coronal hole(s)

ECH(s):

Equatorial coronal hole(s)

EIS:

EUV Imaging Spectrometer (Culhane et al. 2007b)

EIT:

EUV Imaging Telescope (Delaboudinière et al. 1995)

EUV:

Extreme ultraviolet

EUVI:

Extreme UV Imager (Wuelser et al. 2004)

FOV:

Field of view

Hinode :

Solar-B pre-launch (Kosugi et al. 2007)

HMI:

Helioseismic and Magnetic Imager (Scherrer et al. 2012)

HXR(s):

Hard X-ray(s)

IRIS :

Interface Region Imaging Spectrometer (de Pontieu et al. 2014b)

ISSI:

International Space Science Institute, Bern, Switzerland

JBP(s):

Jet-base bright point(s)

LASCO:

Large Angle and Spectrometer COronagraph (Brueckner et al. 1995)

LOS:

Line of sight

MDI:

Michelson Doppler Imager (Scherrer et al. 1995)

MHD:

Magnetohydrodynamic

PCH(s):

Polar coronal hole(s)

QS:

Quiet Sun

RHESSI :

Reuven Ramaty High Energy Solar Spectroscopic Imager (Lin et al. 2002)

SDO :

Solar Dynamics Observatory (Pesnell et al. 2012)

SECCHI:

Sun Earth Connection Coronal and Heliospheric Investigation (Howard et al. 2008)

SOHO :

Solar and Heliospheric Observatory (Domingo et al. 1995)

STEREO :

Solar TErrestrial RElations Observatory (Kaiser et al. 2008)

SUMER:

Solar UV Measurements of Emitted Radiation spectrometer (Wilhelm et al. 1995)

SW:

Solar wind

SXR(s):

Soft X-ray(s)

SXT:

Soft X-ray Telescope (Tsuneta et al. 1991)

TRACE :

Transition Region And Coronal Explorer (Handy et al. 1999)

UV:

Ultraviolet

UVCS:

UV Coronagraph Spectrometer (Kohl et al. 1995)

WL:

White light

XRT:

X-ray Telescope (Golub et al. 2007)

Yohkoh :

Solar-A pre-launch (Ogawara et al. 1991)

References

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Acknowledgements

The “Solar Jets” team members are grateful for the International Space Science Institute (ISSI, Bern, Switzerland) that hosted two meetings on March 2013 and March 2014 within the frame of the international team on the “Solar Coronal Jets (http://www.issibern.ch/teams/solarjets)”. This work benefited greatly from discussions held at these meetings. S. Patsourakos acknowledges support from an FP7 Marie Curie Grant (FP7-PEOPLE-2010-RG/268288) as well as European Union (European Social Fund—ESF) and Greek national funds through the Operational Program “Education and Lifelong Learning” of the National Strategic Reference Framework (NSRF)—Research Funding Program: Thales. Investing in knowledge society through the European Social Fund. A.C. Sterling thanks R.L. Moore for useful discussions. A.C. Sterling was supported by funding from the Heliophysics Division of NASA’s Science Mission Directorate through the Living With a Star Targeted Research and Technology Program, and by funding from the Hinode Project Office at NASA/MSFC. P.R. Young acknowledges funding from National Science Foundation grant AGS-1159353. T. Török was supported by NASA’s HSR and LWS programs. K. Dalmasse acknowledges support from the Computational and Information Systems Laboratory and from the HAO, as well as support from the AFOSR under award FA9550-15-1-0030.

The SOHO is a mission of international cooperation between ESA and NASA. Hinode is a Japanese mission developed and launched by ISAS/JAXA, with NAOJ as a domestic partner and NASA and STFC (UK) as international partners. It is operated by these agencies in cooperation with the ESA and NSC (Norway). The STEREO/SECCHI data used here are produced by an international consortium of the NRL (USA), LMSAL (USA), NASA GSFC (USA), RAL (UK), Univ. Birmingham (UK), MPS (Germany), CSL (Belgium), IOTA (France), and IAS (France). SDO is the first mission to be launched for NASA’s Living With a Star (LWS) Program. IRIS is a NASA small explorer mission developed and operated by LMSAL with mission operations executed at NASA Ames Research center and major contributions to downlink communications funded by the Norwegian Space Center (NSC, Norway) through an ESA PRODEX contract.

Author information

Affiliations

  1. The Johns Hopkins University Applied Physics Laboratory, Laurel, MD, 20723, USA

    N. E. Raouafi

  2. Department of Physics, University of Ioannina, Ioannina, Greece

    S. Patsourakos

  3. LESIA, Observatoire de Paris, Meudon, France

    E. Pariat & K. Dalmasse

  4. College of Science, George Mason University, Fairfax, VA, USA

    P. R. Young

  5. NASA/Goddard Space Flight Center, Code 671, Greenbelt, MD, 20771, USA

    P. R. Young

  6. NASA/Marshall Space Flight Center, Huntsville, AL, USA

    A. C. Sterling

  7. Harvard-Smithsonian Center for Astrophysics, Cambridge, MA, USA

    A. Savcheva

  8. National Astronomical Observatory of Japan, Mitaka, Tokyo, Japan

    M. Shimojo

  9. Instituto de Astrofísica de Canarias, La Laguna, Tenerife, Spain

    F. Moreno-Insertis

  10. Heliophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD, USA

    C. R. DeVore

  11. School of Mathematics and Statistics, University of St. Andrews, St. Andrews, UK

    V. Archontis

  12. Predictive Science Inc., 9990 Mesa Rim Rd., Ste. 170, San Diego, CA, 92121, USA

    T. Török

  13. DAMTP, Centre for Mathematical Sciences, University of Cambridge, Cambridge, UK

    H. Mason

  14. Max-Planck-Institut für Sonnensystemforschung, Göttingen, Germany

    W. Curdt

  15. Division of Computing and Mathematics, Abertay University, Dundee, UK

    K. Meyer

  16. CISL/HAO, NCAR, P.O. Box 3000, Boulder, CO, 80307-3000, USA

    K. Dalmasse

  17. Department of Earth and Planetary Science, University of Tokyo, Tokyo, Japan

    Y. Matsui

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  1. N. E. Raouafi
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  2. S. Patsourakos
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  3. E. Pariat
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  4. P. R. Young
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  5. A. C. Sterling
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  6. A. Savcheva
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  7. M. Shimojo
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  8. F. Moreno-Insertis
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  9. C. R. DeVore
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  10. V. Archontis
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  11. T. Török
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  12. H. Mason
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  13. W. Curdt
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  14. K. Meyer
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  15. K. Dalmasse
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  16. Y. Matsui
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Corresponding author

Correspondence to N. E. Raouafi.

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Raouafi, N.E., Patsourakos, S., Pariat, E. et al. Solar Coronal Jets: Observations, Theory, and Modeling. Space Sci Rev 201, 1–53 (2016). https://doi.org/10.1007/s11214-016-0260-5

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Keywords

  • Plasmas
  • Sun: activity
  • Sun: corona
  • Sun: magnetic fields
  • Sun: UV radiation
  • Sun: X-rays