Space physics

Space physics is the study of the natural phenomenon that occur in our solar system. Specifically, the sun, the particles and radiation it creates and how these affect the planets. This includes the solar wind and its interaction with the Earth and near-Earth space; so-called space weather.

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Latest Research and Reviews

  • Research | | open

    Intense electromagnetic impulses induced by Jupiter’s lightning can produce both low-frequency dispersed whistler emissions and non-dispersed radio pulses. Here, the authors show Jupiter dispersed pulses associated with Jovian lightning that are evidence of low density holes in Jupiter’s ionosphere.

    • Masafumi Imai
    • , Ivana Kolmašová
    • , William S. Kurth
    • , Ondřej Santolík
    • , George B. Hospodarsky
    • , Donald A. Gurnett
    • , Shannon T. Brown
    • , Scott J. Bolton
    • , John E. P. Connerney
    •  & Steven M. Levin
  • Research | | open

    Magnetohydrodynamic (MHD) waves and plasma instabilities can be studied during solar flares. Here the authors show evidence for an MHD sausage mode oscillation periodically triggering electron acceleration at a magnetic null point in the solar corona, indicating MHD oscillations in plasma can indirectly lead to loss-cone instability modulation.

    • Eoin P. Carley
    • , Laura A. Hayes
    • , Sophie A. Murray
    • , Diana E. Morosan
    • , Warren Shelley
    • , Nicole Vilmer
    •  & Peter T. Gallagher
  • Research |

    The merger of two white dwarfs created a massive, hot, luminous, rotating and magnetized star with a lifetime of several thousand years, which will collapse into a type Ic supernova.

    • Vasilii V. Gvaramadze
    • , Götz Gräfener
    • , Norbert Langer
    • , Olga V. Maryeva
    • , Alexei Y. Kniazev
    • , Alexander S. Moskvitin
    •  & Olga I. Spiridonova
    Nature 569, 684-687
  • Research |

    Using large-aperture Cherenkov telescopes, Benbow et al. have measured the angular sizes of two stars through timely occultations by asteroids, achieving an order of magnitude improvement in resolution over the lunar occultation method.

    • W. Benbow
    • , R. Bird
    • , A. Brill
    • , R. Brose
    • , A. J. Chromey
    • , M. K. Daniel
    • , Q. Feng
    • , J. P. Finley
    • , L. Fortson
    • , A. Furniss
    • , G. H. Gillanders
    • , C. Giuri
    • , O. Gueta
    • , D. Hanna
    • , J. P. Halpern
    • , T. Hassan
    • , J. Holder
    • , G. Hughes
    • , T. B. Humensky
    • , A. M. Joyce
    • , P. Kaaret
    • , P. Kar
    • , N. Kelley-Hoskins
    • , M. Kertzman
    • , D. Kieda
    • , M. Krause
    • , M. J. Lang
    • , T. T. Y. Lin
    • , G. Maier
    • , N. Matthews
    • , P. Moriarty
    • , R. Mukherjee
    • , D. Nieto
    • , M. Nievas-Rosillo
    • , S. O’Brien
    • , R. A. Ong
    • , N. Park
    • , A. Petrashyk
    • , M. Pohl
    • , E. Pueschel
    • , J. Quinn
    • , K. Ragan
    • , P. T. Reynolds
    • , G. T. Richards
    • , E. Roache
    • , C. Rulten
    • , I. Sadeh
    • , M. Santander
    • , G. H. Sembroski
    • , K. Shahinyan
    • , I. Sushch
    • , S. P. Wakely
    • , R. M. Wells
    • , P. Wilcox
    • , A. Wilhelm
    • , D. A. Williams
    •  & T. J. Williamson
    Nature Astronomy 3, 511-516

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