Synchrotron emission from double-peaked radio light curves of the symbiotic recurrent nova V3890 Sagitarii
Synchrotron emission from double-peaked radio light curves of the symbiotic recurrent nova V3890 Sagitarii
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共生循环新星 V3890 Sagitarii 双峰射电光变曲线的同步辐射
DOI：
10.1093/mnras/stad1534
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发表时间：
2023
影响因子：
4.8
通讯作者：
Sarbadhicary, Sumit K.
中科院分区：
文献类型：
--
作者：
Nyamai, Miriam M.;Linford, Justin D.;Allison, James R.;Chomiuk, Laura;Woudt, Patrick A.;Ribeiro, Valério A. R. M.;Sarbadhicary, Sumit K.
我们目前的无线电观测共生复发新星V3890射手座在2019年8月爆发后获得的MeerKAT射电望远镜在1.28 GHz和卡尔G。Janksy甚大阵列（VLA），1.26−35 GHz。射电光变曲线从爆发后的第1天到540天，主要是由膨胀的新星喷出物与双星系统中一个进化的伴星的稠密风相互作用产生的同步辐射。无线电发射在早期（第6天）被检测到，并在第15天迅速增加到峰值。射电光度的增加是由于在受冲击物质前面的星周物质的不透明度的降低，并随着周围介质的密度降低和冲击波速度的减速而减弱。通过对光变曲线的模拟，估计红巨星星星的质量损失率为${\overset{\hbox{$}}，而从白色矮星表面喷出的物质质量在Mej = 10−5--10 6 M之间。V3890 Sgr可能拥有一颗巨大的白色矮星，类似于其他共生的复发新星，因此被认为是Ia型超新星（SNe Ia）的候选祖先。然而，它的射电通量密度与超新星Ia的上限相比，排除了它是SN 2011 fe类超新星的祖先。
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 1.26−35 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 ${\overset{\hbox{$ from the red giant star and ejecta mass in the range ofMej= 10−5––10−6M⊙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 like supernovae.
银河新星
DOI：
10.1007/978-94-009-3753-6_16
发表时间：
1987
期刊：
Astrophysics and space science library
影响因子：
--
作者：
S. Starrfield;M. Snijders
通讯作者：
M. Snijders
RS Ophiuchi (2006) 和反复出现的新星现象：在英国基尔基尔大学举办的研讨会论文集
DOI：
--
发表时间：
2008
期刊：
影响因子：
--
作者：
A. Evans
通讯作者：
A. Evans