Cometary X-rays: line emission cross sections for multiply-charged solar wind ion charge exchange

S. OTRANTO, R. E. OLSON, P. BEIERSDORFER

JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS

Insitute of Physics

Lugar: Londres; Año: 2007 vol. 40 p. 1755 - 1766

0953-4075

Absolute line emission cross sections are presented for 1 keV amu-1 charge exchange collisions of multiply charged solar wind ions with H2O. These cross sections can be used to model charge-exchange processes with cometary targets with similar binding energies such as H, O, CO2 and CO. A parameter free model is used to successfully predict the recently observed x-ray spectra of comet Linear C/1999 S4 and McNaught-Hartley C/1999 T1. We show that the resulting spectrum is extremely sensitive to the time variations of the solar wind composition.-1 charge exchange collisions of multiply charged solar wind ions with H2O. These cross sections can be used to model charge-exchange processes with cometary targets with similar binding energies such as H, O, CO2 and CO. A parameter free model is used to successfully predict the recently observed x-ray spectra of comet Linear C/1999 S4 and McNaught-Hartley C/1999 T1. We show that the resulting spectrum is extremely sensitive to the time variations of the solar wind composition.2O. These cross sections can be used to model charge-exchange processes with cometary targets with similar binding energies such as H, O, CO2 and CO. A parameter free model is used to successfully predict the recently observed x-ray spectra of comet Linear C/1999 S4 and McNaught-Hartley C/1999 T1. We show that the resulting spectrum is extremely sensitive to the time variations of the solar wind composition.2 and CO. A parameter free model is used to successfully predict the recently observed x-ray spectra of comet Linear C/1999 S4 and McNaught-Hartley C/1999 T1. We show that the resulting spectrum is extremely sensitive to the time variations of the solar wind composition./1999 S4 and McNaught-Hartley C/1999 T1. We show that the resulting spectrum is extremely sensitive to the time variations of the solar wind composition.