Synchrotron emission from double-peaked radio light curves of the symbiotic recurrent nova V3890 Sagitarii
arXiv:2301.09116 · doi:10.1093/mnras/stad1534
Abstract
We present radio observations of the symbiotic recurrent nova V3890 Sagitarii following the 2019 August eruption obtained with the MeerKAT radio telescope at 1.28 GHz and Karl G. Janksy Very Large Array (VLA) at 1.26 to 5 GHz. The radio light curves span from day 1 to 540 days after eruption and are dominated by synchrotron emission produced by the expanding nova ejecta interacting with the dense wind from an evolved companion in the binary system. The radio emission is detected early on (day 6) and increases rapidly to a peak on day 15. The radio luminosity increases due to a decrease in the opacity of the circumstellar material in front of the shocked material and fades as the density of the surrounding medium decreases and the velocity of the shock decelerates. Modelling the light curve provides an estimated mass-loss rate of from the red giant star and ejecta mass in the range of from the surface of the white dwarf. V3890 Sgr likely hosts a massive white dwarf similar to other symbiotic recurrent novae, thus considered a candidate for supernovae type Ia (SNe Ia) progenitor. However, its radio flux densities compared to upper limits for SNe Ia have ruled it out as a progenitor for SN 2011fe.
References in corpus (31)
- WSClean: an implementation of a fast, generic wide-field imager for radio astronomy
- Circumstellar Emission from Type Ib and Ic Supernovae
- Gamma-Ray Emission Concurrent with the Nova in the Symbiotic Binary V407 Cygni
- X-Ray Emitting Blast Wave from the Recurrent Nova RS Ophiuchi
- An asymmetric shock wave in the 2006 outburst of the recurrent nova RS Ophiuchi
- The Super-Soft X-ray Phase of Nova RS Ophiuchi 2006
- 3D simulations of RS Oph: from accretion to nova blast
- Spectroscopic orbits and variations of RS Oph
- An Expanding Shell and Synchrotron Jet in RS Ophiuchi
- Early spectral evolution of classical novae: consistent evidence for multiple distinct outflows
- Three-dimensional modeling of the asymmetric blast wave from the 2006 outburst of RS Ophiuchi: Early X-ray emission
- Shock evolution in non-radiative supernova remnants
- Measuring the distance to the black hole candidate X-ray binary MAXI J1348-630 using HI absorption
- The Deepest Radio Observations of Nearby Type IA Supernovae: Constraining Progenitor Types and Optimizing Future Surveys
- Near-IR studies of recurrent nova V745 Scorpii during its 2014 outburst
- Classical Novae at Radio Wavelengths
- Double radio peak and non-thermal collimated ejecta in RS Ophiuchi following the 2006 outburst
- Swift observations of the 2006 outburst of the recurrent nova RS Ophiuchi: II. 1D hydrodynamical models of wind driven shocks
- Origin of asymmetries in X-ray emission lines from the blast wave of the 2014 outburst of nova V745 Sco
- Chandra High Energy Transmission Gratings Spectra of V3890 Sgr
- Study of 2021 outburst of the recurrent nova RS Ophiuchi: Photoionization and morpho-kinematic modelling
- The symbiotic recurrent nova V3890 Sgr: binary parameters and pre-outburst activity
- The 2019 eruption of recurrent nova V3890 Sgr: observations by Swift, NICER and SMARTS
- Optical spectroscopy of the recurrent nova RS Ophiuchi - from the outburst of 2006 to quiescence
- A MeerKAT Survey of Nearby Novalike Cataclysmic Variables
- Radio light curves and imaging of the helium nova V445 Puppis reveal seven years of synchrotron emission
- Interpretation of the light curve of GeV-TeV emission from the 2021 outburst of the recurrent nova RS Ophiuchi
- AstroSat Soft X-ray observations of the symbiotic recurrent nova V3890 Sgr during its 2019 outburst
- Infrared spectroscopy of the 2019 eruption of the recurrent nova V3890 Sgr: separation into equatorial and polar winds revealed
- The recurrent nova V3890~Sgr: a near-infrared and optical study of the red giant component and its environment
- Historic mass loss from the RS Ophiuchi system