Cosmic ray heating of intergalactic medium: patchy or uniform?. Issue 1 (7th June 2018)

• Record Type: Journal Article
• Authors: Jana, Ranita; Nath, Biman B
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 479:Issue 1(2018)
• Page Start: 153
• Page End: 161
• Publication Date: 2018-06-07
• Subjects: supernovae: general -- cosmic rays -- intergalactic medium -- dark ages, reionization, first stars; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/sty1481
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: We study the heating of the intergalactic medium (IGM) surrounding high redshift star-forming galaxies due to cosmic rays (CR). We take into account the diffusion of low-energy CR and study the patchiness of the resulting heating. We discuss the case of IGM heating around a high redshift minihalo ($z$ ∼ 10–20, M ∼ 10 5 –10 7 M⊙ ) and put an upper limit on the diffusion coefficient D ≤ 1 × 10 26 cm 2 s −1 for the heating to be inhomogeneous at $z$ ∼ 10 and D ≤ 5–6 × 10 26 cm 2 s −1 at $z$ ∼ 20. For typical values of D, our results suggest uniform heating by CR at high redshift, although there are uncertainties in magnetic field and other CR parameters. We also discuss two cases with continuous star formation, one in which the star formation rate (SFR) of a galaxy is high enough to make the IGM in the vicinity photoionized, and another in which the SFR is low enough to keep it neutral but high enough to cause significant heating by CR protons. In the neutral case (low SFR), we find that the resulting heating can make the gas hotter than the cosmic microwave background radiation for D < 10 30 cm 2 s −1, within a few kpc of the galaxy, and unlikely to be probed by near future radio observations. In the case of photoionized IGM (high SFR), the resulting heating of the gas in the vicinity of high redshift ($z$ ∼ 4) galaxies of mass ≥ 10 12 M⊙ can suppress gas infall into the galaxy. At lower redshifts ($z$ ∼ 0), an SFR of ∼1 M⊙ yr −1 can suppress the infall into galaxies of mass ≤10 10 M⊙ .