Motivated by the recent finding of hierarchical X-ray flaring phenomenon in Mrk 421, we conducted a systematic search for X-ray flares from Mrk 501, another well-known TeV blazar, by making use of the rich RXTE archival database. We detected flares over a wide range of timescales, from months down to minutes, as in the case of Mrk 421. However, the flares do not seem to occur nearly as frequent...

We review the observational, theoretical, and numerical efforts to interpret the statistical behavior of solar flares and sub-flares, and their role to coronal heating. The observed X-ray flares cannot heat the corona. The role of smaller-scale events is still inconclusive, although very recent observational evidence may shed light to the controversy. Statistical and classical modeling reproduc...

Global gas flaring harms human and non-human health well-being while contributing to climate change. Flaring activity in the global oil sector is a significant matter of energy justice – concerning distribution risks, benefits harms, recognition rights, decision-making influence within gas-flaring-affected communities. This mixed method empirical ethical analysis combines Q-methodology stakehol...

Abstract The analysis of light variation M87 can help us understand the disc evolution. In past decade, has experienced several short-term variabilities related to flares. We also find there are year-scale X-ray variations in core M87. Their variability properties similar clumpy-ADAF. By re-analyzing 56 Chandra observations from 2007 2019, we distinguish ‘non-flaring state’ ‘flaring variability...

Isolated Herbig Ae stars can be divided into two groups (Meeus et al. 2001): those with an almost flat spectral energy distribution in the mid-infrared (‘group I’), and those with a strong decline towards the farinfrared (‘group II’). In this paper we show that the group I vs. II distinction can be understood as arising from flaring vs. self-shadowed disks. We show that these two types of disks...

We have re-analyzed using a hydrodynamic model large flaring events on three different categories of pre-main sequence (PMS) stars: the young stellar object (YSO) YLW15, the classical T Tauri star (CTTS) LkHα 92, the weak-line T Tauri star (WTTS) V773 Tau, and the WTTS HD 283572 (the first three objects were observed by ASCA, the last by ROSAT; all have been previously reported in the literatur...

We present optical, X-ray, high energy (/ 30 GeV) and very high energy (' 100 GeV; VHE) observations of the high-frequency peaked blazar Mrk 421 taken between 2008 May 24 and June 23. A high energy γ-ray signal was detected by AGILE with √ TS = 4.5 on June 9–15, with F (E > 100 MeV) = 42 −12 × 10 photons cm s. This flaring state is brighter than the average flux observed by EGRET by a factor of...

Flaring of waste gases is a common practice in the processing of hydrocarbon (HC) materials. It is assumed that flaring achieves complete combustion with relatively innocuous byproducts such as CO2 and H2O. However, flaring is rarely successful in the attainment of complete combustion, because entrainment of air into the region of combusting gases restricts flame sizes to less than optimum valu...

The hydromedusan jellyfish Aglantha digitale feeds on small planktonic organisms carried to the margin by tentacle flexions. During feeding, the manubrium bends across ("points") and seizes the prey with flared lips. In immobilized preparations, pointing to a source of electrical stimulation was accurate, 70% of the time, to within 15 degrees. Cutting experiments showed that the conduction path...

We present a long (150 ks elapsed time) X-ray observation of the dM3.5e star EV Lac, performed with the ASCA observatory in July 1998, during which an exceptionally intense flaring event (lasting approximately 12 ks) was observed: at the flare’s peak, the X-ray count rate in the ASCA GIS detectors was ' 300 times the quiescent value. The physical parameters of the flaring region have been deriv...