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dc.contributor.authorFurlanetto, Steven
dc.contributor.authorLoeb, Abraham
dc.contributor.authorFurlanetto, Steven
dc.contributor.authorLoeb, Abraham
dc.date.accessioned2019-09-24T12:04:35Z
dc.date.issued2003
dc.identifier.citationFurlanetto, Steven R., and Abraham Loeb. 2004. “Large‐Scale Structure Shocks at Low and High Redshifts.” The Astrophysical Journal 611 (2): 642–54. https://doi.org/10.1086/422242.
dc.identifier.issn0004-637X
dc.identifier.issn1538-4357
dc.identifier.urihttp://nrs.harvard.edu/urn-3:HUL.InstRepos:41393344*
dc.description.abstractCosmological simulations show that, at the present time, a substantial fraction of the gas in the intergalactic medium (IGM) has been shock heated to T greater than or similar to 10(5) K. Here we develop an analytic model to describe the fraction of shocked, moderately overdense gas in the IGM. The model is an extension of the Press & Schechter description for the mass function of halos: we assume that large-scale structure shocks occur at a fixed overdensity during nonlinear collapse. This in turn allows us to compute the fraction of gas at a given redshift that has been shock heated to a specified temperature. We show that if strong shocks occur at turnaround, our model provides a reasonable description of the temperature distribution seen in cosmological simulations at z similar to 0, although it does overestimate the importance of weak shocks. We then apply our model to shocks at high redshifts. We show that before reionization, the thermal energy of the IGM is dominated by large-scale structure shocks ( rather than virialized objects). These shocks can have a variety of effects, including stripping less than or similar to10% of the gas from dark matter minihalos, accelerating cosmic rays, and creating a diffuse radiation background from inverse Compton and cooling radiation. This radiation background develops before the first stars form and could have measurable effects on molecular hydrogen formation and the spin temperature of the 21 cm transition of neutral hydrogen. Finally, we show that shock heating will also be directly detectable by redshifted 21 cm measurements of the neutral IGM in the young universe.
dc.language.isoen_US
dc.publisherAmerican Astronomical Society
dash.licenseLAA
dc.titleLarge-Scale Structure Shocks at Low and High Redshifts
dc.typeJournal Article
dc.description.versionAccepted Manuscript
dc.relation.journalThe Astrophysical Journal
dash.depositing.authorLoeb, Abraham::9975df1f269ab49c1ad5a328a1ec1476::600
dc.date.available2019-09-24T12:04:35Z
dash.workflow.comments1Science Serial ID 96515
dc.identifier.doi10.1086/422242
dash.source.volume611;2
dash.source.page642-654


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