Relaxation phenomena in electron plasma of semiconductors

Sokolovsky, S. А.; Sokolovsky, A. I.; Hrinishyn, O. A.

doi:10.15421/332003

Cited by 1 publication

(1 citation statement)

References 3 publications

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“…Following previous multi-wavelength observations (Aydi et al 2020b; Li et al 2020; Drake et al 2020; Sokolovsky et al 2020; Izzo et al 2020), we measured a detection for YZ Ret on 2022 February 6 at frequencies 2.9/5.5/9 GHz with the ATCA (Gulati et al 2022b). In this epoch, the peak radio flux density is somewhere between 2.9 and 9 GHz ( ; ), which indicates that the emission is a mix of optically thick and optically thin thermal emission.…”

Section: Resultsmentioning

confidence: 86%

Classical novae in the ASKAP pilot surveys

Ashna

Murphy

Kaplan

et al. 2023

Publ. Astron. Soc. Aust.

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We present a systematic search for radio counterparts of novae using the Australian Square Kilometer Array Pathfinder (ASKAP). Our search used the Rapid ASKAP Continuum Survey, which covered the entire sky south of declination $+41^{\circ}$ ( $\sim$ $34000$ square degrees) at a central frequency of 887.5 MHz, the Variables and Slow Transients Pilot Survey, which covered $\sim$ $5000$ square degrees per epoch (887.5 MHz), and other ASKAP pilot surveys, which covered $\sim$ 200–2000 square degrees with 2–12 h integration times. We crossmatched radio sources found in these surveys over a two–year period, from 2019 April to 2021 August, with 440 previously identified optical novae, and found radio counterparts for four novae: V5668 Sgr, V1369 Cen, YZ Ret, and RR Tel. Follow-up observations with the Australian Telescope Compact Array confirm the ejecta thinning across all observed bands with spectral analysis indicative of synchrotron emission in V1369 Cen and YZ Ret. Our light-curve fit with the Hubble Flow model yields a value of $1.65\pm 0.17 \times 10^{-4} \rm \:M_\odot$ for the mass ejected in V1369 Cen. We also derive a peak surface brightness temperature of $250\pm80$ K for YZ Ret. Using Hubble Flow model simulated radio lightcurves for novae, we demonstrate that with a 5 $\sigma$ sensitivity limit of 1.5 mJy in 15-min survey observations, we can detect radio emission up to a distance of 4 kpc if ejecta mass is in the range $10^{-3}\rm \:M_\odot$ , and upto 1 kpc if ejecta mass is in the range $10^{-5}$ – $10^{-3}\rm \:M_\odot$ . Our study highlights ASKAP’s ability to contribute to future radio observations for novae within a distance of 1 kpc hosted on white dwarfs with masses $0.4$ – $1.25\:\rm M_\odot$ , and within a distance of 4 kpc hosted on white dwarfs with masses $0.4$ – $1.0\:\rm M_\odot$ .

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