The Sgr B2 X-ray echo of the galactic center supernova explosion that produced Sgr A east

Christopher L. Fryer, Gabriel Rockefeller, Aimee Hungerford, Fulvio Melia

Research output: Contribution to journalArticle

19 Citations (Scopus)

Abstract

Using a combination of one-dimensional and three-dimensional hydrodynamic simulations, we have carried out the first in-depth analysis of the remnant's evolution and its various interactions: with the stellar winds flowing out from the inner ∼2 pc; with the supermassive black hole, Sgr A*; and with the 50 km s-1 molecular cloud behind and to the east of the nucleus. We have found that, unlike previous estimates, a rather "standard" supernova explosion with energy ∼1.5 × 1051 ergs would have been sufficient to create the remnant we see today and that the latter is probably only ∼1700 yr old. We have found that the passage of the remnant across the black hole would have enhanced the accretion rate onto the central object by less than a factor of 2. Such a small increase cannot explain the current Fe fluorescence observed from the molecular cloud Sgr B2; this fluorescence would have required an increase in the luminosity of Sgr A* by 6 orders of magnitude several hundred years ago. Instead, we have uncovered what appears to be a more plausible scenario for this transient irradiation: the interaction between the expanding remnant and the 50 km s-1 molecular cloud. The first impact would have occurred about 1200 yr after the explosion, producing a 2-200 keV luminosity of ∼1039 ergs s -1. During the intervening 300-400 yr, the dissipation of kinetic energy subsided considerably, leading to the much lower luminosity (∼10 36 ergs s-1 at 2-10 keV) we see today.

Original languageEnglish (US)
Pages (from-to)786-796
Number of pages11
JournalAstrophysical Journal
Volume638
Issue number2 I
DOIs
StatePublished - Feb 20 2006

Fingerprint

molecular clouds
erg
supernovae
explosions
explosion
echoes
luminosity
fluorescence
x rays
stellar winds
kinetic energy
dissipation
irradiation
hydrodynamics
accretion
interactions
nuclei
estimates
simulation
energy

Keywords

  • Acceleration of particles
  • Galaxy: center
  • Radiation mechanisms: nonthermal stars: winds, outflows
  • Supernova remnants
  • X-rays: diffuse background

ASJC Scopus subject areas

  • Space and Planetary Science

Cite this

The Sgr B2 X-ray echo of the galactic center supernova explosion that produced Sgr A east. / Fryer, Christopher L.; Rockefeller, Gabriel; Hungerford, Aimee; Melia, Fulvio.

In: Astrophysical Journal, Vol. 638, No. 2 I, 20.02.2006, p. 786-796.

Research output: Contribution to journalArticle

Fryer, Christopher L. ; Rockefeller, Gabriel ; Hungerford, Aimee ; Melia, Fulvio. / The Sgr B2 X-ray echo of the galactic center supernova explosion that produced Sgr A east. In: Astrophysical Journal. 2006 ; Vol. 638, No. 2 I. pp. 786-796.
@article{5e6d83c36c364d8eb8d9f4f3ac10ec40,
title = "The Sgr B2 X-ray echo of the galactic center supernova explosion that produced Sgr A east",
abstract = "Using a combination of one-dimensional and three-dimensional hydrodynamic simulations, we have carried out the first in-depth analysis of the remnant's evolution and its various interactions: with the stellar winds flowing out from the inner ∼2 pc; with the supermassive black hole, Sgr A*; and with the 50 km s-1 molecular cloud behind and to the east of the nucleus. We have found that, unlike previous estimates, a rather {"}standard{"} supernova explosion with energy ∼1.5 × 1051 ergs would have been sufficient to create the remnant we see today and that the latter is probably only ∼1700 yr old. We have found that the passage of the remnant across the black hole would have enhanced the accretion rate onto the central object by less than a factor of 2. Such a small increase cannot explain the current Fe fluorescence observed from the molecular cloud Sgr B2; this fluorescence would have required an increase in the luminosity of Sgr A* by 6 orders of magnitude several hundred years ago. Instead, we have uncovered what appears to be a more plausible scenario for this transient irradiation: the interaction between the expanding remnant and the 50 km s-1 molecular cloud. The first impact would have occurred about 1200 yr after the explosion, producing a 2-200 keV luminosity of ∼1039 ergs s -1. During the intervening 300-400 yr, the dissipation of kinetic energy subsided considerably, leading to the much lower luminosity (∼10 36 ergs s-1 at 2-10 keV) we see today.",
keywords = "Acceleration of particles, Galaxy: center, Radiation mechanisms: nonthermal stars: winds, outflows, Supernova remnants, X-rays: diffuse background",
author = "Fryer, {Christopher L.} and Gabriel Rockefeller and Aimee Hungerford and Fulvio Melia",
year = "2006",
month = "2",
day = "20",
doi = "10.1086/498968",
language = "English (US)",
volume = "638",
pages = "786--796",
journal = "Astrophysical Journal",
issn = "0004-637X",
publisher = "IOP Publishing Ltd.",
number = "2 I",

}

TY - JOUR

T1 - The Sgr B2 X-ray echo of the galactic center supernova explosion that produced Sgr A east

AU - Fryer, Christopher L.

AU - Rockefeller, Gabriel

AU - Hungerford, Aimee

AU - Melia, Fulvio

PY - 2006/2/20

Y1 - 2006/2/20

N2 - Using a combination of one-dimensional and three-dimensional hydrodynamic simulations, we have carried out the first in-depth analysis of the remnant's evolution and its various interactions: with the stellar winds flowing out from the inner ∼2 pc; with the supermassive black hole, Sgr A*; and with the 50 km s-1 molecular cloud behind and to the east of the nucleus. We have found that, unlike previous estimates, a rather "standard" supernova explosion with energy ∼1.5 × 1051 ergs would have been sufficient to create the remnant we see today and that the latter is probably only ∼1700 yr old. We have found that the passage of the remnant across the black hole would have enhanced the accretion rate onto the central object by less than a factor of 2. Such a small increase cannot explain the current Fe fluorescence observed from the molecular cloud Sgr B2; this fluorescence would have required an increase in the luminosity of Sgr A* by 6 orders of magnitude several hundred years ago. Instead, we have uncovered what appears to be a more plausible scenario for this transient irradiation: the interaction between the expanding remnant and the 50 km s-1 molecular cloud. The first impact would have occurred about 1200 yr after the explosion, producing a 2-200 keV luminosity of ∼1039 ergs s -1. During the intervening 300-400 yr, the dissipation of kinetic energy subsided considerably, leading to the much lower luminosity (∼10 36 ergs s-1 at 2-10 keV) we see today.

AB - Using a combination of one-dimensional and three-dimensional hydrodynamic simulations, we have carried out the first in-depth analysis of the remnant's evolution and its various interactions: with the stellar winds flowing out from the inner ∼2 pc; with the supermassive black hole, Sgr A*; and with the 50 km s-1 molecular cloud behind and to the east of the nucleus. We have found that, unlike previous estimates, a rather "standard" supernova explosion with energy ∼1.5 × 1051 ergs would have been sufficient to create the remnant we see today and that the latter is probably only ∼1700 yr old. We have found that the passage of the remnant across the black hole would have enhanced the accretion rate onto the central object by less than a factor of 2. Such a small increase cannot explain the current Fe fluorescence observed from the molecular cloud Sgr B2; this fluorescence would have required an increase in the luminosity of Sgr A* by 6 orders of magnitude several hundred years ago. Instead, we have uncovered what appears to be a more plausible scenario for this transient irradiation: the interaction between the expanding remnant and the 50 km s-1 molecular cloud. The first impact would have occurred about 1200 yr after the explosion, producing a 2-200 keV luminosity of ∼1039 ergs s -1. During the intervening 300-400 yr, the dissipation of kinetic energy subsided considerably, leading to the much lower luminosity (∼10 36 ergs s-1 at 2-10 keV) we see today.

KW - Acceleration of particles

KW - Galaxy: center

KW - Radiation mechanisms: nonthermal stars: winds, outflows

KW - Supernova remnants

KW - X-rays: diffuse background

UR - http://www.scopus.com/inward/record.url?scp=33644756730&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=33644756730&partnerID=8YFLogxK

U2 - 10.1086/498968

DO - 10.1086/498968

M3 - Article

VL - 638

SP - 786

EP - 796

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 2 I

ER -