论文标题
MWC 297的多波长观测：磁盘倾斜度和质量流出的约束
Multi-wavelength Observations of MWC 297: Constraints on Disk Inclination and Mass Outflow
论文作者
论文摘要
MWC 297是一位年轻的早期型明星，驾驶电离流出，周围是温暖，夹带的灰尘。先前对近红外和中期干涉图像的分析表明，这些波长处的发射来自中等（$ i <40美元）倾斜度的紧凑型积聚盘。我们已经在索非亚上获得了5-40微米的MWC 297图像，以及在IRTF上使用SPEX获得的近红外光谱和使用VLA和BIMA获得的无线电数据，并用Herschel/Pacs和Spire的档案数据补充了这些档案数据。前播图像与VLA数据结合使用，表明流出叶几乎向北对齐，并且分离良好。预播图像的简单几何建模表明，驱动流出的磁盘的倾向为$ 55 \ pm 5 $度，与干涉分析的结果不同意。通过风模型对SPEX数据的分析表明，质量损失率在$ 6.0 \ pm^{3.7} _ {1.7} _ {1.7} \ times 10^{ - 7} m_ \ odot〜 \ odot〜 \ mathrm {yr} \ pm^{2.5} _ {1.5} $ mag。我们已经将数据与文献的值结合在一起，以产生源的光谱能量分布从$ 0.35〜μm到$ 6 $ cm，并估计总发光度。如果我们在恒星周围的扩展区域中包括少于B1.5V星的预期，我们发现总的亮度约为7900 〜l_ \ odot $。沿视线沿尘埃产生的红色必须产生，但远离星星。
MWC 297 is a young, early-type star driving an ionized outflow and surrounded by warm, entrained dust. Previous analyses of near- and mid-IR interferometric images suggest that the emission at these wavelengths arises from a compact accretion disk with a moderate ($i < 40$ degrees) inclination. We have obtained 5-40 micron images of MWC 297 with FORCAST on SOFIA, as well as near-infrared spectra acquired with SpeX on the IRTF and radio data obtained with the VLA and BIMA, and supplemented these with archival data from Herschel/PACS and SPIRE. The FORCAST images, combined with the VLA data, indicate that the outflow lobes are aligned nearly north-south and are well separated. Simple geometrical modeling of the FORCAST images suggests that the disk driving the outflow has an inclination of $55\pm 5$ degrees, in disagreement with the results of the interferometric analyses. Analysis of the SpeX data, with a wind model, suggests the the mass loss rate is on the order of $6.0 \pm ^{3.7}_{1.7} \times 10^{-7} M_\odot ~\mathrm{yr}^{-1}$ and the extinction to the source is $A_V \sim 8.1 \pm^{2.5}_{1.5}$ mag. We have combined our data with values from the literature to generate the spectral energy distribution of the source from $0.35~ μ$m to $6$ cm and estimate the total luminosity. We find the total luminosity to be about $7900 ~ L_\odot$, if we include emission from an extended region around the star, only slightly below that expected for a B1.5V star. The reddening must be produced by dust along the line of sight, but distant from the star.
