Results 41 to 50 of about 1,350,678 (342)
Migration of Solar Polar Crown Filaments in the Past 100 Years
, 2021 Polar crown filaments (PCFs) are formed above the polarity inversion line, which separates unipolar polar fields and the nearest dispersed fields. They are important features in studying solar polar fields and their cyclical variations.
Yan Xu +7 more
semanticscholar +1 more source
Commission 10: Solar Activity [PDF]
, 2007 Commission 10 aims at the study of various forms of solar activity, including networks, plages, pores, spots, fibrils, surges, jets, filaments/prominences, coronal loops, flares, coronal mass ejections (CMEs), solar cycle, microflares, nanoflares ...
Benz, A.O. +10 more
core +2 more sources
Tilt Angles of Solar Filaments over the Period of 1919 – 2014 [PDF]
, 2016 The spatial and temporal distributions of solar filaments were analyzed using data from the Meudon Observatory for the period of 1919 – 2003 and the Kislovodsk Mountain Astronomical Station for the period of 1979 – 2014. We scanned Hα$\mathrm{H}\upalpha$
A. Tlatov +2 more
semanticscholar +1 more source
TETHER-CUTTING RECONNECTION BETWEEN TWO SOLAR FILAMENTS TRIGGERING OUTFLOWS AND A CORONAL MASS EJECTION [PDF]
, 2016 Triggering mechanisms of solar eruptions have long been a challenge. A few previous case studies have indicated that preceding gentle filament merging via magnetic reconnection may launch following intense eruption, according to the tether-cutting (TC ...
Huadong Chen +3 more
semanticscholar +1 more source
High-altitude Spider-type Prominence above the Magnetic Null Point
The Astrophysical Journal, 2023 Rather unique observations of a high-altitude spider-type prominence in 2023 February are presented. The prominence or corresponding filament on the disk was not visible all the time but could appear and disappear in the course of a particular day ...
Boris Filippov
doaj +1 more source
Dynamical Mass Estimates of Large-Scale Filaments in Redshift Surveys [PDF]
, 1996 We propose a new method to measure the mass of large-scale filaments in galaxy redshift surveys. The method is based on the fact that the mass per unit length of isothermal filaments depends only on their transverse velocity dispersion.
Abraham Loeb +13 more
core +3 more sources
, 2015 We improve our filament automated detection method which was proposed in our previous works. It is then applied to process the full disk H$\alpha$ data mainly obtained by Big Bear Solar Observatory (BBSO) from 1988 to 2013, spanning nearly 3 solar cycles.
Cao, W., Chen, P. F., Fang, C., Hao, Q.
core +1 more source
Sympathetic Partial Filament Eruptions Caused by the Interaction between Two Nearby Filaments
The Astrophysical Journal, 2023 To better understand the physical connections in sympathetic solar eruptions, we investigated the interaction between two nearby filaments and their successive partial eruptions in the active region (AR) NOAA 12866 on 2021 September 9 by using data from ...
Liping Yang +9 more
doaj +1 more source
The Astrophysical Journal, 2023 Although magnetic reconnection plays a key role in the formation of a solar filament, the detailed formation process is still ambiguous. Combining the observational data from the New Vacuum Solar Telescope and the Solar Dynamics Observatory, we analyzed ...
Liping Yang +9 more
doaj +1 more source
On rotation of solar filaments [PDF]
Proceedings of the International Astronomical Union, 2006 The study of the differential rotation law is an important issue in solar physics. Earlier studies of filaments found formulae for their differential rotation at stable existence stage. This paper relies on Big Bear Solar Observatory H-alpha filtergrams to estimate angular velocities of quiescent filaments at different stages of existence.
openaire +1 more source