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    Wyświetlanie 1-3 z 3
    Tytuł:
    Numerical simulations of impulsively excited fast magnetosonic waves in two parallel slabs
    Autorzy:
    Ogrodowczyk, R.
    Murawski, K.
    Powiązania:
    https://bibliotekanauki.pl/articles/1955342.pdf
    Data publikacji:
    2006
    Wydawca:
    Politechnika Gdańska
    Tematy:
    Sun: MHD
    Sun: corona
    Sun: oscillation
    Opis:
    We present numerical results of a temporal evolution of impulsively excited magnetosonic waves in a solar coronal loop that is approximated by a set of two straight plasma slabs of mass density enhancement. Numerical simulations reveal that shapes of wavelet spectra of time signatures of these waves depend on a distance between the strands and on a position of the initial pulse. We find that with a distance growing between these strands short period waves contribute more while long period waves contribute less to the wavelet spectra. We demonstrate that a presence of the second parallel strand affects considerably wave propagation in comparison to one strand alone. We find out that the initial pulse triggers a packet of propagating waves among witch sausage and kink modes are present simultaneously.
    Źródło:
    TASK Quarterly. Scientific Bulletin of Academic Computer Centre in Gdansk; 2006, 10, 3; 227-238
    1428-6394
    Pojawia się w:
    TASK Quarterly. Scientific Bulletin of Academic Computer Centre in Gdansk
    Dostawca treści:
    Biblioteka Nauki
    Artykuł
    Tytuł:
    Numerical simulations of slow magneto sonic standing waves in a two-dimensional hot solar coronal slab
    Autorzy:
    Ogrodowczyk, R.
    Murawski, K.
    Powiązania:
    https://bibliotekanauki.pl/articles/1933175.pdf
    Data publikacji:
    2007
    Wydawca:
    Politechnika Gdańska
    Tematy:
    sun
    solar corona
    MHD oscillations
    Opis:
    We consider impulsive excitation of slow magnetosonic standing waves in a two-dimensional hot solar coronal slab. Results of numerical simulations have revealed that initially launched pulses trigger mainly fundamental slow mode and its first harmonic, depending on the pulses' spatial location. Our parametric study has shown these slow standing waves to exhibit wave periods of about 13min. The slow standing waves are accompanied by fast modes simultaneously present in the system.
    Źródło:
    TASK Quarterly. Scientific Bulletin of Academic Computer Centre in Gdansk; 2007, 11, 3; 263-271
    1428-6394
    Pojawia się w:
    TASK Quarterly. Scientific Bulletin of Academic Computer Centre in Gdansk
    Dostawca treści:
    Biblioteka Nauki
    Artykuł
    Tytuł:
    An X-ray Observations of A Gradual Coronal Mass Ejections (CMEs) on 15th April 2012
    Autorzy:
    Hamidi, Z. S.
    Shariff, N. N. M.
    Monstein, C.
    Wan Zulkifli, W. N. A.
    Ibrahim, M. B.
    Arifin, N. S.
    Amran, N. A.
    Powiązania:
    https://bibliotekanauki.pl/articles/411850.pdf
    Data publikacji:
    2014
    Wydawca:
    Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
    Tematy:
    Sun Coronal Mass Ejections (CMEs)
    solar corona
    solar flare
    solar cycle
    Opis:
    In the present work, we will highlight the solar observation during 15th April 2012, solar filament eruption which is accompanied by an intense and gradual Coronal Mass Ejections (CMEs) The explosion of CMEs was observed at 2:12:06 UT and also can be observed by the Solar Dynamics Observatory (SDO) with an Active Region AR1458 is crackling with C-class solar flares. The solar flare class B3 and C2 were observed beginning 2241 UT and 0142 UT. The event is considered as second largest CMEs been detected since five years. Although the solar activity within a few days is considered quite low and there are no proton events were observed at geosynchronous orbit., the is still an unexpected explosion of CMEs can be occurred. The radio flux number (10.7 cm) exceeds 102 with the number of sunspot and area of sunspot increased to 77 and 270. The velocity of CMEs was calculated based on the LASCO2 data. From the results, it is clearly seen that the range of the velocity is between 200 kms-1 to 2000 kms-1. This wide of range proved that the mechanism of the CMEs is a gradual process. The explosion of CMEs velocity is located from 80º - 255º from North of the Sun. We can then conclude that currently, the rearrangement of the magnetic field, and solar flares may result in the formation of a shock that accelerates particles ahead of the CMEs loop and an active region play an important character in this event.
    Źródło:
    International Letters of Chemistry, Physics and Astronomy; 2014, 8; 13-19
    2299-3843
    Pojawia się w:
    International Letters of Chemistry, Physics and Astronomy
    Dostawca treści:
    Biblioteka Nauki
    Artykuł
      Wyświetlanie 1-3 z 3

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