Matches in SemOpenAlex for { <https://semopenalex.org/work/W2290790711> ?p ?o ?g. }
- W2290790711 endingPage "66" @default.
- W2290790711 startingPage "44" @default.
- W2290790711 abstract "Several supernovae (SNe) with an unusually dense circumstellar medium (CSM) have been recently observed at radio frequencies. Their radio emission is powered by relativistic electrons that can be either accelerated at the SN shock (primaries) or injected as a by-product (secondaries) of inelastic proton–proton collisions. We investigate the radio signatures from secondary electrons, by detailing a semi-analytical model to calculate the temporal evolution of the distributions of protons, primary and secondary electrons. With our formalism, we track the cooling history of all the particles that have been injected into the emission region up to a given time, and calculate the resulting radio spectra and light curves. For an SN shock propagating through the progenitor wind, we find that secondary electrons control the early radio signatures, but their contribution decays faster than that of primary electrons. This results in a flattening of the light curve at a given radio frequency that depends only upon the radial profiles of the CSM density and of the shock velocity, υ0. The relevant transition time at the peak frequency is |${sim } {190} , {rm d} , K_{rm ep,-3}^{-1} A_{rm w, 16}{/beta _{0, -1.5}^2}$|, where Aw is the wind mass-loading parameter, β0 = υ0/c and Kep are the electron-to-proton ratio of accelerated particles. We explicitly show that late peak times at 5 GHz (i.e. tpk ≳ 300–1000 d) suggest a shock wave propagating in a dense wind (Aw ≳ 1016–1017 gr cm−1), where secondary electrons are likely to power the observed peak emission." @default.
- W2290790711 created "2016-06-24" @default.
- W2290790711 creator A5032765567 @default.
- W2290790711 creator A5078054206 @default.
- W2290790711 creator A5091459136 @default.
- W2290790711 date "2016-04-21" @default.
- W2290790711 modified "2023-10-17" @default.
- W2290790711 title "Radio synchrotron emission from secondary electrons in interaction-powered supernovae" @default.
- W2290790711 cites W1481709258 @default.
- W2290790711 cites W1511284520 @default.
- W2290790711 cites W1518078371 @default.
- W2290790711 cites W1552565640 @default.
- W2290790711 cites W1808840155 @default.
- W2290790711 cites W1891118963 @default.
- W2290790711 cites W1923156118 @default.
- W2290790711 cites W1963998371 @default.
- W2290790711 cites W1964331461 @default.
- W2290790711 cites W1969101649 @default.
- W2290790711 cites W1969941231 @default.
- W2290790711 cites W1975584241 @default.
- W2290790711 cites W1976316526 @default.
- W2290790711 cites W1977925093 @default.
- W2290790711 cites W1978188911 @default.
- W2290790711 cites W1979569506 @default.
- W2290790711 cites W1981217972 @default.
- W2290790711 cites W1981279573 @default.
- W2290790711 cites W1982292118 @default.
- W2290790711 cites W1986956674 @default.
- W2290790711 cites W1988045362 @default.
- W2290790711 cites W1989756559 @default.
- W2290790711 cites W1990535341 @default.
- W2290790711 cites W1994303408 @default.
- W2290790711 cites W1995255005 @default.
- W2290790711 cites W2000494005 @default.
- W2290790711 cites W2001741999 @default.
- W2290790711 cites W2005094094 @default.
- W2290790711 cites W2007322325 @default.
- W2290790711 cites W2007403924 @default.
- W2290790711 cites W2008354954 @default.
- W2290790711 cites W2010232869 @default.
- W2290790711 cites W2011634292 @default.
- W2290790711 cites W2012738214 @default.
- W2290790711 cites W2018829983 @default.
- W2290790711 cites W2019332977 @default.
- W2290790711 cites W2022119466 @default.
- W2290790711 cites W2022279921 @default.
- W2290790711 cites W2023668546 @default.
- W2290790711 cites W2032167309 @default.
- W2290790711 cites W2032882333 @default.
- W2290790711 cites W2034683667 @default.
- W2290790711 cites W2038848106 @default.
- W2290790711 cites W2039365614 @default.
- W2290790711 cites W2044989047 @default.
- W2290790711 cites W2048673059 @default.
- W2290790711 cites W2049024396 @default.
- W2290790711 cites W2052788604 @default.
- W2290790711 cites W2053287308 @default.
- W2290790711 cites W2053570386 @default.
- W2290790711 cites W2054152824 @default.
- W2290790711 cites W2054185545 @default.
- W2290790711 cites W2054923548 @default.
- W2290790711 cites W2058798168 @default.
- W2290790711 cites W2064057617 @default.
- W2290790711 cites W2064831009 @default.
- W2290790711 cites W2066355200 @default.
- W2290790711 cites W2067971031 @default.
- W2290790711 cites W2069414247 @default.
- W2290790711 cites W2072362373 @default.
- W2290790711 cites W2073564169 @default.
- W2290790711 cites W2076666077 @default.
- W2290790711 cites W2080948533 @default.
- W2290790711 cites W2081160630 @default.
- W2290790711 cites W2082987405 @default.
- W2290790711 cites W2084297519 @default.
- W2290790711 cites W2085701755 @default.
- W2290790711 cites W2089647157 @default.
- W2290790711 cites W2091057992 @default.
- W2290790711 cites W2091166540 @default.
- W2290790711 cites W2092165725 @default.
- W2290790711 cites W2095319512 @default.
- W2290790711 cites W2098012226 @default.
- W2290790711 cites W2099966304 @default.
- W2290790711 cites W2100702882 @default.
- W2290790711 cites W2106891871 @default.
- W2290790711 cites W2117832995 @default.
- W2290790711 cites W2127318216 @default.
- W2290790711 cites W2130897264 @default.
- W2290790711 cites W2131981030 @default.
- W2290790711 cites W2141354567 @default.
- W2290790711 cites W2142542912 @default.
- W2290790711 cites W2145652018 @default.
- W2290790711 cites W2149809013 @default.
- W2290790711 cites W2153154960 @default.
- W2290790711 cites W2159833008 @default.
- W2290790711 cites W2160527048 @default.
- W2290790711 cites W2163812193 @default.
- W2290790711 cites W2166503936 @default.
- W2290790711 cites W2167098062 @default.