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Browsing by Author "Doddamani, V. H"

Browsing by Author "Doddamani, V. H"

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  • Coronal hole oscillations inferred from the SDO/AIA data 
    Hegde, M; Hiremath, K. M; Doddamani, V. H (Elsevier B.V, 2014-07-15)
    With high temporal resolution (12 sec) of about two hours duration, data of a coronal hole structure in 171°A, 193°A and 211°A taken from SDO/AIA images is considered for examination of oscillations. After estimating the ...
  • Finding the Critical Decay Index in Solar Prominence Eruptions 
    Vasantharaju, N.; Vemareddy, P; Ravindra, B; Doddamani, V. H (IOP Publishing, 2019-11)
    The background fi eld is assumed to play a prime role in erupting structures like prominences. In the fl ux rope models, the critical decay index ( n c ) is a measure of the rate at which background fi eld ...
  • Formation and eruption of sigmoidal satructure from a weak field region of NOAA 11942 
    Vasantharaju, N; Vemareddy, P; Ravindra, B; Doddamani, V. H (IOP Publishing, 2019-04-01)
    Using observations from the Solar Dynamics Observatory, we studied an interesting example of a sigmoid formation and eruption from small-scale flux-canceling regions of active region (AR) 11942. Through an analysis of ...
  • Magnetic Imprints of Eruptive and Noneruptive Solar Flares as Observed by Solar Dynamics Observatory 
    Vasantharaju, N; Vemareddy, P; Ravindra, B; Doddamani, V. H (American Astronomical Society, 2022-03-01)
    The abrupt and permanent changes of the photospheric magnetic field in the localized regions of active regions during solar flares, called magnetic imprints (MIs), have been observed for nearly the past three decades. The ...
  • Recurring coronal holes and their rotation rates during the solar cycles 22-24 
    Prabhu, K; Ravindra, B; Hegde, M; Doddamani, V. H (Springer, 2018-05)
    Coronal holes (CHs) play a significant role in making the Earth geo-magnetically active during the declining and minimum phases of the solar cycle. In this study, we analysed the evolutionary characteristics of the Recurring ...
  • Segmentation of Coronal Features to Understand the Solar EUV and UV Irradiance Variability 
    Kumara, S. T; Kariyappa, R; Zender, J. J; Giono, G; Delouille, V; Pradeep Chitta, L; Dame, L; Hochedez, J. F; Verbeeck, C; Mampaey, B; Doddamani, V. H (EDP Sciences, 2014-01)
    Context. The study of solar irradiance variability is of great importance in heliophysics, the Earth’s climate, and space weather applications. These studies require careful identifying, tracking and monitoring of active ...
  • Solar wind associated with near equatorial coronal Hole 
    Hegde, M; Hiremath, K. M; Doddamani, V. H; Gurumath, S. R (2015-09)
    Present study probes temporal changes in the area and radiative flux of near equatorial coronal hole associated with solar wind parameters such as wind speed, density, magnetic field and temperature. Using high temporal ...
  • Spectroscopic study of the Carbon-Enhanced Metal-Poor star: HE 0110-0406 
    Meenakshi, P; Goswami, A; Doddamani, V. H (Societe Royale des Sciences de Liege, 2019-10)
    The halo system of the Milky way comprises the vast majority of the presently observed metal-poor ([Fe/H] <1.0) and very metal-poor ([Fe/H] <2.0) stars. A sizable fraction (~ 30%) of the metal-poor stars with carbon ...
  • Statistical Study of Magnetic Nonpotential Measures in Confined and Eruptive Flares 
    Vasantharaju, N; Vemareddy, P; Ravindra, B; Doddamani, V. H (IOP Publishing, 2018-06-10)
    Using Solar Dynamics Observatory/Helioseismic and Magnetic Imager vector magnetic field observations, we studied the relation between the degree of magnetic non-potentiality with the observed flare/coronal mass ejection ...
  • UVIT observation of Milky Way satellite galaxy Reticulum II 
    Divakar, D. K; Sivarani, T; Doddamani, V. H (Indian Academy of Sciences, 2021-10)
    We present the UV photometry of one of the Ultra-Faint Dwarf (UFD) Milky Way (MW) satellite galaxies, Reticulum II, using images acquired with the Ultra-Violet Imaging Telescope (UVIT) onboard AstroSat. Reticulum II is ...

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