2015
DOI: 10.1088/0004-637x/809/1/79
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Connecting Flares and Transient Mass-Loss Events in Magnetically Active Stars

Abstract: We explore the ramification of associating the energetics of extreme magnetic reconnection events with transient mass loss in a stellar analogy with solar eruptive events. We establish energy partitions relative to the total bolometric radiated flare energy for different observed components of stellar flares, and show that there is rough agreement for these values with solar flares. We apply an equipartition between the bolometric radiated flare energy and kinetic energy in an accompanying mass ejection, seen … Show more

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Cited by 145 publications
(189 citation statements)
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References 66 publications
(113 reference statements)
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“…This work built on earlier theoretical models of time-steady solar wind scaling relations (Cranmer & Saar 2011) and on empirical correlations between CME properties and highenergy flare emissions (e.g., Aarnio et al 2012;Drake et al 2013;Osten & Wolk 2015). Although it is likely that the magnetic properties of a star are more fundamental (i.e., they are what drive the flare and CME properties), it is also undeniable that they are much more difficult to observe than, say, flare light curves.…”
Section: Discussionmentioning
confidence: 99%
“…This work built on earlier theoretical models of time-steady solar wind scaling relations (Cranmer & Saar 2011) and on empirical correlations between CME properties and highenergy flare emissions (e.g., Aarnio et al 2012;Drake et al 2013;Osten & Wolk 2015). Although it is likely that the magnetic properties of a star are more fundamental (i.e., they are what drive the flare and CME properties), it is also undeniable that they are much more difficult to observe than, say, flare light curves.…”
Section: Discussionmentioning
confidence: 99%
“…From their Table 2, we estimate the bolometric radiated energy two ways: using the extrapolated U-band energy described above, as well as the X-ray energies calculated in Section 3.3.1. The estimation of bolometric energy using the coronal radiated energy is imprecise because the formulation of Osten & Wolk (2015) only considered the 0.01-10 keV energy range, whereas the BFF event clearly has significant contribution at higher photon energies. The two estimates of bolometric energy differ from each other by a factor of threeor more.…”
Section: Energy Partition In Bff and F2 And Estimates Of Totalmentioning
confidence: 99%
“…The amount of energy radiated in the V filter bandpass is about an order of magnitude less than this. Section 3.3.4 discusses the energy partition within BFF and F2; both appear to be X-ray luminous compared to expectations from scaling of optical flare energy to bolometric radiated energy from Osten & Wolk (2015). The integrated V-band energy from the EVLac superflare described in Osten et al (2010) could not be calculated due to insufficient data, but we note that the large enhancement flare on the very-low-mass star described in Stelzer et al (2006) had nearly equal amounts of radiated energy in the X-ray and V filter bandpasses (but overall lower integrated values, at ∼3×10 32 erg).…”
Section: Interpretation Of Bffmentioning
confidence: 99%
“…(Drake et al, 2013) made comparisons of solar power-law relationships to stellar energies to extrapolate what mass loss may be possible from solar-like stars. It is clear that there is potential for significant mass loss (see also Osten and Wolk, 2015).…”
Section: Implications For Cmes From Other Starsmentioning
confidence: 99%