TY - JOUR
T1 - A 149 min periodicity underlies the X-ray flaring of Sgr A*
AU - Leibowitz, Elia
N1 - Publisher Copyright:
© 2017 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society.
PY - 2018/3/1
Y1 - 2018/3/1
N2 - In a paper in 2017, I have shown that 39 large X-ray flares of Sgr A* that were recorded by Chandra observatory in the year 2012 are concentrated preferably around tick marks of an equi-distance grid on the time axis. The period of this grid as found in that paper is 0.1033 d. In this work I show that the effect can be found among all the large X-ray flares recorded by Chandra and XMM - Newton along 15 yr. The mid-points of all the 71 large flares recorded between years 2000 and 2014 are also tightly grouped around tick marks of a grid with this period, or more likely, 0.1032 d. This result is obtained with a confidence level of at least 3.27σ and very likely of 4.62σ. I find also a possible hint that a similar grid is underlying IR flares of the object. I suggest that the pacemaker in the occurrences of the large X-ray flares of Sgr A* is a mass of the order of a low-mass star or a small planet, in a slightly eccentric Keplerian orbit around the SMBH at the centre of the Galaxy. The radius of this orbit is about 6.6 Schwarzschild radii of the BH.
AB - In a paper in 2017, I have shown that 39 large X-ray flares of Sgr A* that were recorded by Chandra observatory in the year 2012 are concentrated preferably around tick marks of an equi-distance grid on the time axis. The period of this grid as found in that paper is 0.1033 d. In this work I show that the effect can be found among all the large X-ray flares recorded by Chandra and XMM - Newton along 15 yr. The mid-points of all the 71 large flares recorded between years 2000 and 2014 are also tightly grouped around tick marks of a grid with this period, or more likely, 0.1032 d. This result is obtained with a confidence level of at least 3.27σ and very likely of 4.62σ. I find also a possible hint that a similar grid is underlying IR flares of the object. I suggest that the pacemaker in the occurrences of the large X-ray flares of Sgr A* is a mass of the order of a low-mass star or a small planet, in a slightly eccentric Keplerian orbit around the SMBH at the centre of the Galaxy. The radius of this orbit is about 6.6 Schwarzschild radii of the BH.
KW - Black hole physics
KW - Galaxy: centre
KW - X-rays: individual: Sgr A
UR - http://www.scopus.com/inward/record.url?scp=85040239503&partnerID=8YFLogxK
U2 - 10.1093/mnras/stx2939
DO - 10.1093/mnras/stx2939
M3 - ???researchoutput.researchoutputtypes.contributiontojournal.article???
AN - SCOPUS:85040239503
SN - 0035-8711
VL - 474
SP - 3380
EP - 3390
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 3
ER -