X-rays from the Local Bubble

Details X-rays from the Local Bubble X-rays from the Local Bubble

Feb 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004ap%26ss.289..229f&link_type=abstract

Astrophysics and Space Science, v. 289, Issue 3, p. 229-238 (2004).

Astronomy and Astrophysics

Astrophysics

2

Local Bubble, Local Interstellar Medium, Galactic Halo, Diffuse X-Ray Emission, Xmm-Newton Mission

Scientific paper

Thermal plasma emission in the soft X-ray band (0.1 2.0 keV)is believed to be responsible for the bulk of the X-ray intensityseen from the Local Bubble, a low-density cavity extending over˜ 70 200 pc around the Sun. The state of the hot plasmais still a matter of discussion as previous instrumentation like aboardROSAT was not able to unambiguously distinguish betweenequilibrium and non-equilibrium emission models and thus topin-point the origin of the Local Bubble. Recent missions like DXS, XQC, and XMM-Newton have shed more lighton this subject and observations indicate that collisional ionizationequilibrium with solar abundances cannot explain the data: lines appear at positions and with intensities in contradictionto standard models. Analysis of EPIC-pn data of X-ray shadowing observations (MBM 12,Ophiuchus molecular cloud) suggest a componentwith higher temperature (kT˜ 0.14 keV) besides thestandard kT˜ 0.09 keV plasma.

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