Zobrazeno 1 - 10
of 901
pro vyhledávání: '"Solar spicules"'
Autor:
Sadeghi, R., Tavabi, E.
Solar winds originate from the Sun and can be classified as fast or slow. Fast solar winds come from coronal holes at the solar poles, while slow solar winds may originate from the equatorial region or streamers. Spicules are jet-like structures obse
Externí odkaz:
http://arxiv.org/abs/2408.07168
Publikováno v:
A&A 689, A135 (2024)
Propagating (intensity) disturbances (PDs) are well reported in observations of coronal loops and polar plumes in addition to recent links with co-temporal spicule activity in the solar atmosphere. However, despite being reported in observations, the
Externí odkaz:
http://arxiv.org/abs/2406.16577
Autor:
Saleem, Hamid, Saleem, Zain H.
Physical mechanism for the creation of solar spicules is proposed with three stages of their life cycle. It is assumed that at stage-I, the density hump is formed locally in the xy-plane in lower chromosphere in the presence of temperature gradients
Externí odkaz:
http://arxiv.org/abs/2307.14328
Autor:
Dey, Sahel, Chatterjee, Piyali, N., Murthy O. V. S., Korsos, Marianna B., Liu, Jiajia, Nelson, Christopher J., Erdelyi, Robertus
Spicules are plasma jets, observed in the dynamic interface region between the visible solar surface and the hot corona. At any given time, it is estimated that about 3 million spicules are present on the Sun. We find an intriguing parallel between t
Externí odkaz:
http://arxiv.org/abs/2211.04493
Akademický článek
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Autor:
Iwazaki, Aiichi
It has recently been observed that solar spicules covering almost of all solar surface have strong magnetic field $B\sim 10^2$G. They are supposed to be plasma jets emitted from chromosphere and they arrive up to $\sim 10^4$km. Their electron number
Externí odkaz:
http://arxiv.org/abs/2206.07866
Autor:
Hamid Saleem, Zain H. Saleem
Publikováno v:
The Astrophysical Journal, Vol 967, Iss 1, p 9 (2024)
The physical mechanism for the creation of solar spicules is proposed with three stages of their life cycle. It is assumed that at stage I the density hump is formed locally in the x-y plane in the lower chromosphere in the presence of temperature gr
Externí odkaz:
https://doaj.org/article/2809f1a58e254b73923b1b4ca4dd2977
Akademický článek
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Publikováno v:
A&A 642, A61 (2020)
Aims. We use high-resolution spectropolarimetric observations in the Ca ii 8542 A line obtained with the SST to study the magnetic field in solar spicules. Methods. The equations that result from the application of the Weak Field Approximation (WFA)
Externí odkaz:
http://arxiv.org/abs/2006.01809
We examine Big Bear Solar Observatory (BBSO) Goode Solar Telescope (GST) high-spatial resolution (0''.06), high-cadence (3.45 s), H-alpha-0.8 Angstrom images of central-disk solar spicules, using data of Samanta et al. (2019). We compare with coronal
Externí odkaz:
http://arxiv.org/abs/2004.04187