Heavy Coronal Ions in the Heliosphere: I. Global Distribution of Charge-states of C, N, O, Mg, Si and S

Details Heavy Coronal Ions in the Heliosphere: I. Global Distribution of Charge-states of C, N, O, Mg, Si and S Heavy Coronal Ions in the Heliosphere: I. Global Distribution of Charge-states of C, N, O, Mg, Si and S

2008-08-22

arxiv.org/abs/0808.3102v2

Astronomy and Astrophysics

Astrophysics

Reduced-resolution version, submitted to A&A; full resolution: http://articles.cbk.waw.pl/0printed/g/grzedzielski_etal08a.pdf.

Scientific paper

Aims: Investigate/Study de-charging of solar wind C, N, O, Mg, Si and S ions and assess fluxes of resulting ENA in the heliosphere. Methods: The model treats the heavy ions as test particles convected by (and in a particular case also diffusing through) a hydrodynamically calculated background plasma flow, from 1 AU to the termination shock (TS), to heliosheath (HS) and finally to heliospheric tail (HT). The ions undergo radiative and dielectronic recombinations, charge exchanges, photo- and electron impact ionizations with plasma particles, interstellar neutral atoms (calculated on a Monte-Carlo model) and solar photons. Results: Highly-charged heavy coronal ions flowing with the solar wind undergo successive de-ionizations, mainly in the heliosheath, leading to charge-states much lower than in the supersonic solar wind. If Coulomb scattering is the main ion energy loss mechanism, the end product of these deionizations are fluxes of ENA of ~1 keV/nucleon originating in the upwind heliosheath that for C, Mg, Si and S may constitute sources of pickup ions (PUI) significantly exceeding the interstellar supply. Conclusions: Discussed processes result in (i) distinct difference of ion charge q in the supersonic solar wind (approximately q >= +Z/2, Z = atomic number) compared to that in the HS (approximately 0 <= q <= +Z/2)), (ii) probable concentration of singly ionized atoms (q = +1) in the heliosheath towards the heliopause (HP) and in the HT, (iii) possible significant production of ENA in the HS offering natural explanation for production of PUI, and -- after acceleration at the TS -- anomalous cosmic rays (ACR) of species (like C, Mg, Si, S) unable to enter the heliospheric cavity from outside because of their total ionization in the local interstellar medium.

Affiliated with

Also associated with

No associations

Rating

Heavy Coronal Ions in the Heliosphere: I. Global Distribution of Charge-states of C, N, O, Mg, Si and S does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Heavy Coronal Ions in the Heliosphere: I. Global Distribution of Charge-states of C, N, O, Mg, Si and S, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Heavy Coronal Ions in the Heliosphere: I. Global Distribution of Charge-states of C, N, O, Mg, Si and S will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-185884