Results 51 to 60 of about 27,428 (205)

X-ray flares in Orion young stars. I. Flare characteristics

, 2008
Pre-main sequence (PMS) stars are known to produce powerful X-ray flares which resemble magnetic reconnection solar flares scaled by factors up to 10^4.
Drake J. J., Eric D. Feigelson, Giuseppina Micela, Gordon P. Garmire, Hiei E., Isobe H., Jardine M., Konstantin V. Getman, Patrick S. Broos, Reale F., Reale F., Serio S., Siess L., Sylwester B.   +13 more
core   +1 more source

A Joint Microwave and Hard X-Ray Study toward Understanding the Transport of Accelerated Electrons During an Eruptive Solar Flare

The Astrophysical Journal
The standard flare model, despite its success, is limited in comprehensively explaining the various processes involving nonthermal particles. One such missing ingredient is a detailed understanding of the various processes involved during the transport ...
Surajit Mondal, Andrea F. Battaglia, Bin Chen, Sijie Yu   +3 more
doaj   +1 more source

High-resolution solar flare X-ray spectra

The Astrophysical Journal, 1979
High spectral resolution solar flare spectra have been recorded by four Bragg crystal spectrometers flown by the Naval Research Laboratory on a spacecraft launched 1979 February 24 by the Air Force. The wavelength ranges discussed in the Letter are 1.82--1.97 A, 2.98--3.07 A, and 3.14--3.24 A.
G. A. Doschek, R. W. Kreplin, U. Feldman
openaire   +1 more source

ALEXIS: Recreating the X-Ray Emission from the Full Solar Disk as a Linear Combination of Discrete Regions in the Extreme Ultraviolet and Soft X-Rays

The Astrophysical Journal Supplement Series
Despite a wealth of multiwavelength, spatially resolved, time-domain solar activity data, an accurate and complete temporospatial solar flare census is unavailable, which impedes our understanding of the physics of flare production.
Jorge R. Padial Doble, Kelly Holley-Bockelmann   +1 more
doaj   +1 more source

Using the Maximum X-ray Flux Ratio and X-ray Background to Predict Solar Flare Class

, 2015
We present the discovery of a relationship between the maximum ratio of the flare flux (namely, 0.5-4 Ang to the 1-8 Ang flux) and non-flare background (namely, the 1-8 Ang background flux), which clearly separates flares into classes by peak flux level.
Balasubramaniam, K., Winter, Lisa M.
core   +1 more source

Statistics of X-ray flares of Sagittarius A*: evidence for solar-like self-organized criticality phenomenon [PDF]

, 2015
X-ray flares have routinely been observed from the supermassive black hole, Sagittarius A$^\star$ (Sgr A$^\star$), at our Galactic center. The nature of these flares remains largely unclear, despite of many theoretical models. In this paper, we study the
Chen, P. F., Dexter, Jason, Fang, Taotao, Li, Ya-Ping, Neilsen, Joseph, Wang, Q. Daniel, Yuan, Feng, Yuan, Qiang, Zhang, Shuo   +8 more
core   +2 more sources

X-Ray, Near-ultraviolet, and Optical Flares Produced by Colliding Magnetospheres in the Young High-eccentricity Binary DQ Tau

The Astrophysical Journal, 2023
DQ Tau is a unique young high-eccentricity binary system that exhibits regular magnetic reconnection flares and pulsed accretion near periastron. We conducted NuSTAR, Swift, and Chandra observations during the 2022 July 30 periastron to characterize X ...
Konstantin V. Getman, Ágnes Kóspál, Nicole Arulanantham, Dmitry A. Semenov, Grigorii V. Smirnov-Pinchukov, Sierk E. van Terwisga   +5 more
doaj   +1 more source

The gas pixel detector as a solar X-ray polarimeter and imager

, 2011
The Sun is the nearest astrophysical source with a very intense emission in the X-ray band. The study of energetic events, such as solar flares, can help us to understand the behaviour of the magnetic field of our star.
Bellazzini, Ronaldo, Brez, Alessandro, Costa, Enrico, Di Cosimo, Sergio, Fabiani, Sergio, Lazzarotto, Francesco, Muleri, Fabio, Rubini, Alda, Soffitta, Paolo, Spandre, Gloria   +9 more
core   +1 more source

Searching for Rapid Pulsations in Solar Flare X-Ray Data

The Astrophysical Journal
Most studies of quasiperiodic pulsations (QPPs) in solar flares have identified characteristic periods in the 5–300 s range. Due to observational limitations, there have been few attempts to probe the
Andrew R. Inglis, Laura A. Hayes
doaj   +1 more source

Different Power-law Indices in the Frequency Distributions of Flares with and without Coronal Mass Ejections

, 2006
We investigated the frequency distributions of flares with and without coronal mass ejections (CMEs) as a function of flare parameters (peak flux, fluence, and duration of soft X-ray flares).
Akiyama, S., Gopalswamy, N., Howard, R. A., Yashiro, S.   +3 more
core   +1 more source