论文标题
使用LWA观察100 MHz以下的耀斑星
Observing Flare Stars Below 100 MHz with the LWA
论文作者
论文摘要
我们观察到耀斑恒星Leonis，Wolf 424，Eq Pegasi，Ev Lacertae和UV Ceti近135小时。使用长波长阵列的干涉法模式观察到这些恒星在63至83 MHz之间。鉴于耀斑恒星的发射通常是循环极化的，我们使用了以下条件：Stokes中存在的任何显着检测我也必须同时存在于Stokes V中，以便我们认为这可能是可能的耀斑。此后，我们为星eq Pegasi进行了一个边缘耀斑检测。该耀斑的通量密度为5.91 jy I中的I和Stokes V中的5.13 Jy，对应于亮度温度$ 1.75 \ times 10^{16} {16}（r/r _*）^{ - 2} $K。
We observed the flare stars AD Leonis, Wolf 424, EQ Pegasi, EV Lacertae, and UV Ceti for nearly 135 hours. These stars were observed between 63 and 83 MHz using the interferometry mode of the Long Wavelength Array. Given that emission from flare stars is typically circularly polarized, we used the condition that any significant detection present in Stokes I must also be present in Stokes V at the same time in order for us to consider it a possible flare. Following this, we made one marginal flare detection for the star EQ Pegasi. This flare had a flux density of 5.91 Jy in Stokes I and 5.13 Jy in Stokes V, corresponding to a brightness temperature $1.75 \times 10^{16}(r/r_*)^{-2}$ K.
