Calibrated Estimates of the Energy in Major Flares of GRS 1915+105

TL;DR

This study estimates the energy of a major radio flare from GRS 1915+105, confirming the calibration method's accuracy and its correlation with X-ray luminosity, enhancing understanding of black hole jet energetics.

Contribution

It extends the calibrated flare energy estimation method to a new, highly energetic flare, validating its applicability beyond previous data sets.

Findings

Calibrated energy estimates are accurate for the 2005 flare.

Flare energy correlates with pre- and during-ejection X-ray luminosity.

X-ray luminosity is elevated before and during the ejection event.

Abstract

We analyze the energetics of the major radio flare of October 8 2005 in GRS 1915+105. The flare is of particular interest because it is one of the most luminous and energetic radio flares from a Galactic black hole that has ever been observed. The motivation is two-fold. One, to learn more about the energetics of this most extreme phenomenon and its relationship to the accretion state. The second is to verify if the calibrated estimates of the energy of major radio flares (based on the peak low frequency optically thin flux) derived from flares in the period 1996-2001 in Punsly & Rodriguez (2013), PR13 hereafter, can be used to estimate plasmoid energy beyond this time period. We find evidence that the calibrated curves are still accurate for this strong flare. Furthermore, the physically important findings of PR13 are supported by the inclusion of this flare: the flare energy is correlated with both the intrinsic bolometric X-ray luminosity, $L_{\mathrm{bol}}$, $\sim 1$ hour before ejection and $L_{\mathrm{bol}}$ averaged over the duration of the ejection of the plasmoid and $L_{\mathrm{bol}}$ is highly elevated relative to historic levels just before and during the ejection episode. A search of the data archives reveal that only the October 8 2005 flare and those in PR13 have adequate data sampling to allow estimates of both the energy of the flare and the X-ray luminosity before and during flare launch.