The origin of the local 1/4-keV X-ray flux in both charge exchange and a hot bubble

M. Galeazzi (), M. Chiao, M. R. Collier, T. Cravens, D. Koutroumpa, K. D. Kuntz, R. Lallement, S. T. Lepri, D. McCammon, K. Morgan, F. S. Porter, I. P. Robertson, S. L. Snowden, N. E. Thomas, Y. Uprety, E. Ursino and B. M. Walsh
Additional contact information
M. Galeazzi: University of Miami, Coral Gables, Florida 33124, USA
M. Chiao: NASA Goddard Space Flight Center
M. R. Collier: NASA Goddard Space Flight Center
T. Cravens: University of Kansas
D. Koutroumpa: Université Versailles St Quentin; CNRS/INSU, LATMOS-IPSL, Guyancourt 78280, France
K. D. Kuntz: Johns Hopkins University
R. Lallement: GEPI Observatoire de Paris, CNRS UMR 8111, Université Paris Diderot, 92190, Meudon, France
S. T. Lepri: Oceanic and Space Sciences, University of Michigan
D. McCammon: University of Wisconsin
K. Morgan: University of Wisconsin
F. S. Porter: NASA Goddard Space Flight Center
I. P. Robertson: University of Kansas
S. L. Snowden: NASA Goddard Space Flight Center
N. E. Thomas: NASA Goddard Space Flight Center
Y. Uprety: University of Miami, Coral Gables, Florida 33124, USA
E. Ursino: University of Miami, Coral Gables, Florida 33124, USA
B. M. Walsh: NASA Goddard Space Flight Center

Nature, 2014, vol. 512, issue 7513, 171-173

Abstract: The contribution of solar-wind ions exchanging electrons with helium and hydrogen near the Sun is shown to be only about 40 per cent of the 1/4-keV X-ray flux observed in the Galactic plane; this supports the existence of a local ‘hot bubble’ filled with X-ray-emitting gas, accounting for the rest of the flux.

Date: 2014
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DOI: 10.1038/nature13525

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