SiO Maser Spectra of V407 Cyg after the 2010 March Nova Outburst

TL;DR

This study investigates the evolution of SiO maser emissions in the V407 Cyg system following its 2010 nova outburst, revealing rapid shock effects and subsequent replenishment of the maser regions.

Contribution

It provides the first detailed observational analysis of SiO maser variability in a symbiotic system after a nova event, highlighting shock destruction and recovery processes.

Findings

SiO maser emission was weak but detectable after the outburst.

Line profiles changed dramatically within weeks, indicating shock effects.

Replenishment of maser regions occurs rapidly due to Mira pulsation.

Abstract

We report on the time variation of SiO maser emission from the symbiotic stellar system V407 Cyg after the classical nova outburst on 2010 March 10. Although both the SiO $J=1$--0 $v=1$ and 2 lines at 43.122 and 42.821 GHz were found previously in the envelope of a mira in the binary system, only weak emission of the $J=1$--0 $v=2$ line has continuously been detectable after the nova outburst. The line profile exhibited a dramatic change several weeks after the burst; the component on the higher-velocity side of the systemic velocity disappeared two weeks after the burst, and a new persistent component appeared on the lower-velocity side later. These observations indicate that the SiO emitting regions are wiped out in a time scale of two weeks by the nova shock, but a part of the masing region is quickly replenished by cool molecular gases expelled by the mira pulsation.