Tau Boo行星的磁层辐射：多纪元搜索
Magnetospheric Emissions from the Planet Orbiting tau Boo: A Multi-Epoch Search
摘要：
太阳系中所有的气态巨行星都产生电子回旋脉泽，由撞击其磁层的太阳风驱动。外推到环绕陶博的行星，许多作者预测它可能在甚大阵列上的4米波长（74 MHz）系统的检测范围内。本文报道了Tau Boo的三个观测时期。在任何时期我们都没有探测到这颗行星;各种确定发射上限的方法产生的单时期极限范围从135到300 mJy。我们开发了一种多历元观测的似然方法，并用它来约束行星的各种辐射特性。假设这颗行星确实在我们的观测波长下辐射，它的典型光度必须小于约10 ^{16} W，除非它的辐射被高度光束射入立体角Ω <<1 sr。这个值低于最近的估计，最近的估计试图利用已知的恒星本身的特性来考虑Tau Boo的恒星风。来自太阳系行星的电子回旋脉泽辐射被光束照射，但具有大约1 sr的特征立体角。未来的长波长仪器（例如，长波长阵列和低频阵列）必须能够在短时间尺度（~15分钟）上进行典型的通量密度测量。大约25 mJy，以显著改善这些约束。
英文摘要：
All of the solar system gas giants produce electron cyclotron masers, driven by the solar wind impinging on their magnetospheres. Extrapolating to the planet orbiting tau Boo, various authors have predicted that it may be within the detection limits of the 4-meter wavelength (74 MHz) system on the Very Large Array. This paper reports three epochs of observations of tau Boo. In no epoch do we detect the planet; various means of determining the upper limit to the emission yield single-epoch limits ranging from 135 to 300 mJy. We develop a likelihood method for multi-epoch observations and use it to constrain various radiation properties of the planet. Assuming that the planet does radiate at our observation wavelength, its typical luminosity must be less than about 10^{16} W, unless its radiation is highly beamed into a solid angle Omega << 1 sr. While within the range of luminosities predicted by various authors for this planet, this value is lower than recent estimates which attempt to take into account the stellar wind of tau Boo using the known properties of the star itself. Electron cyclotron maser emission from solar systems planets is beamed, but with characteristic solid angles of approximately 1 sr illuminated. Future long-wavelength instruments (e.g., the Long Wavelength Array and the Low Frequency Array) must be able to make typical flux density measurements on short time scales (~ 15 min.) of approximately 25 mJy in order to improve these constraints significantly.
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