Zobrazeno 1 - 10
of 221
pro vyhledávání: '"Vemareddy A"'
Autor:
Vemareddy, P.
Magnetic flux ropes (FRs) are twisted structures appearing on the sun, predominantly in the magnetically concentrated regions. These structures appear as coronal features known as filaments or prominences in H$\alpha$ observations, and as sigmoids in
Externí odkaz:
http://arxiv.org/abs/2410.02670
Autor:
Vemareddy, P.
Aiming to capture the formation and eruption of flux ropes (FRs) in the source active regions (ARs), we simulate the coronal magnetic field evolution of the AR 11429 employing the time-dependent magneto-friction model (TMF). The initial field is driv
Externí odkaz:
http://arxiv.org/abs/2409.14045
Coronal magnetic fields evolve quasi statically over long time scales and dynamically over short time scales. As of now there exists no regular measurements of coronal magnetic fields, and therefore generating the coronal magnetic field evolution usi
Externí odkaz:
http://arxiv.org/abs/2312.12124
Autor:
Vemareddy, P.
Using multi-instrument and multi-wavelength observations, we studied a CME eruption that led to intense geomagnetic storm on 23 April 2023. The eruption occurred on April 21 in solar active region 13283 near the disk-center. The AR was in its decay s
Externí odkaz:
http://arxiv.org/abs/2312.08790
Autor:
Priyal, Muthu, Singh, Jagdev, Prasad, B. Raghavendra, Sumana, Chavali, Kumar, Varun, Mishra, Shalabh, Venkata, S. N., Sindhuja, G., Raja, K. Sasikumar, Kumar, Amit, krishnan, Sanal, Hegde, Bhavana S., Utkarsha, D., Venkatasubramanian, Natarajan, Somasundram, Pawankumar, Nagabhushana, S., Kamath, PU., Kathiravan, S., Mani, T. Vishnu, Basavaraju, Suresh, Chavan, Rajkumar, Vemareddy, P., Ravindra, B., Rajaguru, S. P., Nagaraju, K., Mishra, Wageesh, Joshi, Jayant, Samanta, Tanmoy, Chatterjee, Piyali, Kathiravan, C., Ramesh, R.
ADITYA-L1 is India's first dedicated mission to observe the sun and its atmosphere from a halo orbit around L1 point. Visible emission line coronagraph (VELC) is the prime payload on board at Aditya-L1 to observe the sun's corona. VELC is designed as
Externí odkaz:
http://arxiv.org/abs/2307.03173
Autor:
Vemareddy, P.
Using time-sequence vector magnetic field and coronal observations from \textit{Solar Dynamics Observatory}, we report the observations of the magnetic field evolution and coronal activity in four emerging active regions (ARs). The ARs emerge with le
Externí odkaz:
http://arxiv.org/abs/2208.03228
Using the observations from Solar Dynamics Observatory, we study an eruption of a hot-channel flux rope (FR) near the solar-limb on February 9, 2015. The pre-eruptive structure is visible mainly in EUV 131 $\mathring{\mathrm{A}}$ images with two high
Externí odkaz:
http://arxiv.org/abs/2201.06899
The abrupt and permanent changes of photospheric magnetic field in the localized regions of active regions during solar flares called magnetic imprints (MIs), have been observed for the past nearly three decades. The well known "coronal implosion" mo
Externí odkaz:
http://arxiv.org/abs/2201.06550
Autor:
Vemareddy, P.
This paper studies the magnetic topology of successively erupting active regions (ARs) 11429 and 12371. Employing vector magnetic field observations from Helioseismic and Magnetic Imager, the pre-eruptive magnetic structure is reconstructed by a mode
Externí odkaz:
http://arxiv.org/abs/2109.14583
Autor:
Vemareddy, P.
Magnetic helicity (MH) is a measure of twist and shear of magnetic field. MH is injected in the active region (AR) corona through photospheric footpoint motions causing twisted and sheared magnetic fields. From the conservation property of the helici
Externí odkaz:
http://arxiv.org/abs/2108.07741