1. RRI Digital Repository
  2. 04. Astronomy and Astrophysics
  3. Research Papers (A&A)
Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/7442
Full metadata record
DC FieldValueLanguage
dc.contributor.authorVijayan, Aditi-
dc.contributor.authorNath, Biman B.-
dc.contributor.authorSharma, Prateek-
dc.contributor.authorShchekinov, Yuri-
dc.date.accessioned2020-03-05T08:34:26Z-
dc.date.available2020-03-05T08:34:26Z-
dc.date.issued2020-02-02-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society, 2020, Vol.492, p2924–2935en_US
dc.identifier.issn0035-8711-
dc.identifier.issn1365-2966 (online)-
dc.identifier.urihttp://hdl.handle.net/2289/7442-
dc.descriptionOpen Access.en_US
dc.description.abstractWe study the synchronous radio emission from extra-planar regions of star-forming galaxies. We use ideal magneto hydrodynamic simulations of a rotating Milky Way-type disc galaxy with distributed star formation sites for three star formation rates (0.3, 3, 30 M☉ yr-1). From our simulations, we see emergence of galactic-scale magnetized outflows, carrying gas from the disc. We compare the morphology of the out flowing gas with hydrodynamic simulations. We look at the spatial distribution of magnetic field in the outflows. Assuming that a certain fraction of gas energy density is converted into cosmic ray energy density, and using information about the magnetic field, we obtain synchronous emissivity throughout the simulation domain. We generate the surface brightness maps at 1.4 GHz. The outflows are more extended in the vertical direction than radial and hence have an oblate shape. We further find that the matter right behind the outer shock shines brighter in these maps than that above or below. To understand whether this feature can be observed, we produce vertical intensity profiles. We convolve the vertical intensity profile with the typical beam sizes of radio telescopes, for a galaxy located at 10 Mpc to estimate the radio scale height and compare with observations. The radio scale height is ∼300-1200 pc, depending on the resolution of the telescope. We relate the advection speed of the outer shock with the surface density of star formation as v_adv ∝ Σ _SFR^{0.3}, which is consistent with earlier observations and analytical estimates.en_US
dc.language.isoenen_US
dc.publisherOxford University Press on behalf of the Royal Astronomical Societyen_US
dc.relation.urihttps://ui.adsabs.harvard.edu/abs/2020MNRAS.492.2924V/abstracten_US
dc.relation.urihttps://arxiv.org/abs/1911.07870en_US
dc.relation.urihttps://doi.org/10.1093/mnras/stz3568en_US
dc.rights2019 The Author(s)en_US
dc.subjectgalaxies: evolutionen_US
dc.subjectgalaxies: haloesen_US
dc.subjectgalaxies: spiralen_US
dc.subjectradio continuum: galaxiesen_US
dc.titleRadio haloes of star-forming galaxiesen_US
dc.typeArticleen_US
Appears in Collections:Research Papers (A&A)

Files in This Item:
File Description SizeFormat 
2020_MNRAS_Vol.492_p2924–2935.pdfOpen Access2.6 MBAdobe PDFView/Open
Show simple item record


Items in RRI Digital Repository are protected by copyright, with all rights reserved, unless otherwise indicated.