CONFIRMATION AND CHARACTERIZATION OF THE PROTOPLANET HD 100546 b—DIRECT EVIDENCE FOR GAS GIANT PLANET FORMATION AT 50 AU
CONFIRMATION AND CHARACTERIZATION OF THE PROTOPLANET HD 100546 b—DIRECT EVIDENCE FOR GAS GIANT PLANET FORMATION AT 50 AU
复制标题
原行星 HD 100546 b 的确认和表征——50 天文单位气态巨行星形成的直接证据
DOI：
10.1088/0004-637x/807/1/64
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发表时间：
2014
期刊：
影响因子：
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通讯作者：
M. Kasper
中科院分区：
文献类型：
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作者：
S. Quanz;A. Amara;M. Meyer;Julien H. Girard;M. Kenworthy;M. Kasper
我们提出了第一个多波长、高对比度的成像研究，证实了嵌入在赫比格Ae/Be恒星HD 100546周围的圆盘中的原行星。该目标在L(∼3.8m？gt；)和M‘(∼4.8m？？gt；)处被探测到，但在Ks(∼2.1m？？gt；)处没有被探测到，并且发射由空间分辨发射所包围的点源分量组成。对于点源分量，我们得到了视震级：L=13.92±0.10；MAG，M‘=13.33±0.16；MAG，K S；15.43±0.06；MAG(3σ极限)，间隔和位置角分别为(0.457±0.014)“和(8.4±1.4)°；和(0.472±0.014)”；L和M‘分别为(9.2±1.4)°和(9.2±1.4)°。我们证明了该天体与HD 100546是同步运动的，并且可以拒绝任何(亚)恒星前景/背景天体。将单温黑体与观测到的点源成分的通量进行拟合，得到有效温度T ff=932−2 2+193？gt；K，发射区半径R=6.9−2.9+2.7？最适光度为L=(2.3−0.4+0.6)·10−4 L⊙？我们将我们的发现与年轻的气态巨行星的演化和大气模型的预测进行了定量比较，讨论了温暖的环行星盘的可能存在，并注意到(53±2)？>；AU的非投影物理分离对标准的行星形成理论构成了挑战。考虑到怀疑在∼13-14 AU轨道上存在另一颗行星，HD 100546似乎是一个史无前例的实验室，可以从经验上研究多个气态巨行星的形成。
We present the first multi-wavelength, high-contrast imaging study confirming the protoplanet embedded in the disk around the Herbig Ae/Be star HD 100546. The object is detected at L′ ( ∼ 3.8 &mgr; m ?> ) and M′ ( ∼ 4.8 &mgr; m ?> ), but not at Ks ( ∼ 2.1 &mgr; m ?> ), and the emission consists of a point source component surrounded by spatially resolved emission. For the point source component we derive apparent magnitudes of L ′ = 13.92 ± 0.10 ?> mag, M ′ = 13.33 ± 0.16 ?> mag, and K s > 15.43 ± 0.06 ?> mag (3σ limit), and a separation and position angle of ( 0.457 ± 0.014 ) ″ ?> and ( 8.4 ± 1.4 ) ° ?> , and ( 0.472 ± 0.014 ) ″ ?> and ( 9.2 ± 1.4 ) ° ?> in L′ and M′, respectively. We demonstrate that the object is co-moving with HD 100546 and can reject any (sub-)stellar fore-/background object. Fitting a single-temperature blackbody to the observed fluxes of the point source component yields an effective temperature of T eff = 932 − 202 + 193 ?> K and a radius for the emitting area of R = 6.9 − 2.9 + 2.7 ?> R Jupiter ?> . The best-fit luminosity is L = ( 2.3 − 0.4 + 0.6 ) · 10 − 4 L ⊙ ?> . We quantitatively compare our findings with predictions from evolutionary and atmospheric models for young, gas giant planets, discuss the possible existence of a warm, circumplanetary disk, and note that the deprojected physical separation from the host star of ( 53 ± 2 ) ?> AU poses a challenge to standard planet formation theories. Considering the suspected existence of an additional planet orbiting at ∼13–14 AU, HD 100546 appears to be an unprecedented laboratory to study the formation of multiple gas giant planets empirically.