Detection of a variable interstellar absorption component towards δ Orionis A     

R. J. Price  I. A. Crawford  M. J. Barlow 《Monthly notices of the Royal Astronomical Society》2000,312(3):L43-L48

Observations of δ Ori A made with the UHRF in its highest resolution mode ( R ≈900 000) have revealed the presence of a cool ( T _k350 K) variable absorption component at a heliocentric velocity of +21.3 km s⁻¹. The component is detected in Na  i D₁, where clear hyperfine splitting is seen, and Ca  ii K. Comparison of our data with existing spectra suggests that the component has consistently increased in strength from 1966 to 1994, and subsequently reduced in intensity by 1999. Following a discussion of the possible origins of this component it is concluded that an interstellar, rather than circumstellar, origin is most likely. This is one of very few detections of variable interstellar absorption reported in the literature, and we suggest an origin within filamentary material associated with the expanding H  i shell surrounding the Orion–Eridanus superbubble.  相似文献   

The southern active-chromosphere star HD 6628     

L. C. Watson  J. B. Hearnshaw  K. R. Pollard  P. M. Kilmartin  A. C. Gilmore 《Monthly notices of the Royal Astronomical Society》2000,315(1):69-76

The star HD 6628, heretofore classified as a G5 subgiant, is shown to be a chromospherically active single-lined spectroscopic binary with a period of 27.332±0.008 d. From high-resolution spectra, the system is found to consist of a late F-type dwarf and an active G8–K1 bright subgiant, the latter having a rotation period of not more than 14.8±3.8 d derived from the width of metal lines. Further stellar and orbital parameters are derived and presented.  相似文献   

基于高分辨率遥感影像的车道线提取     

张世强  王贵山 《测绘通报》2019,(12):22-25

车道线是自动驾驶高精度地图的组成部分，利用车载摄像头和激光雷达提取车道线的研究已经比较深入。本文探讨了利用高分辨率遥感影像提取车道线的方法。首先依据直方图原则选取合适的阈值进行二值化分割，其次利用道路中线形成的缓冲区去除道路范围外的要素，然后利用形态学算子去除噪声，最后利用方向和面积因子提取不同的车道线。该方法可以降低数据采集的成本，提高采集效率。  相似文献   

恒星自转测量中因标准星速度非零所引入误差的讨论     

汪洵浩 《中国天文和天体物理学报》1988,(1)

近年来,谭徽松等人以所选用标准星的观测轮廓与Gray的转致轮廓直接卷积,再与被测星观测轮廓比较,由此来测量了一些恒星的自转。在这种方法中,当所选标准星自转速度不严格为零时,将引入误差。本文在标准星速度(vsini)_s较小的条件下,进行函数展开,先后给出了轮廓修正关系式R_0(λ)=R(λ)-α_2(△λ_L)_s~2R″(λ),及速度修正关系式(vsini)_0~2=(vsini)~2+(vsini)_s~2。并估算说明,当标准星速度(vsini)_s<5km/s,而被测星速度vsini>20km/s时,该误差可不考虑。  相似文献   

Binarity of the red-rectangle and other extremely fe-poor (post?)-AGB stars     

Hans Van Winckel  Christoffel Waelkens 《Astrophysics and Space Science》1995,224(1-2):581-582

We present radial velocity measurements proving the binary nature of all the known extremely Fe-deficient Post-ABG stars including HD 44179, the central star of the well known but poorly understood Red-Rectangle nebula. With the observed orbital parameters, it is more likely that the stars represent a particular stage in binary evolution, rather than a typical post-AGB evolutionary stage.  相似文献   

星风对双星HD698运动的影响     

陈黎  郑学塘 《中国天文和天体物理学报》1991,(2)

本文利用变质量二体问题讨论了由于星风造成的质量减少对双星HD698的轨道的影响。  相似文献   

Photometric, spectroscopic and polarimetric variability of the weak-emission T Tauri star HD 288313     

M. V. Mekkaden  S. Muneer  A. V. Raveendran 《Monthly notices of the Royal Astronomical Society》2007,378(3):1079-1088

Photometric observations over three seasons show HD 288313 to be a light variable with a 2.2636-d period. The observed V amplitudes lie in the range of 0.06–0.15 mag. The star showed appreciable changes in the brightness at maximum and minimum of the light curve from season to season. The (   b − y   ) colour did not show any significant variation during the photometric cycle. The light variation appears to be caused by the rotational modulation of stellar flux by cool starspots distributed asymmetrically across the stellar longitudes. The Hα line strength in HD 288313 varied drastically from completely filled-in emission to almost full absorption, that is typical of a normal star of similar spectral type. The Hα equivalent width is found to show a clear rotational modulation only occasionally. Most of the time, chromospheric active regions are distributed well across the stellar longitudes, thereby suppressing obvious rotational modulations. Broad-band linear polarization measurements show HD 288313 to be a short period, low-amplitude polarization variable. The polarization variation is, apparently, rotationally modulated. Dust grain scattering in a non-spherical circumstellar envelope of a star with inhomogeneities in the surface brightness distribution seems to be the mechanism operating in producing the observed polarization.  相似文献   

PEPSI: The high‐resolution échelle spectrograph and polarimeter for the Large Binocular Telescope     

K.G. Strassmeier  I. Ilyin  A. Jrvinen  M. Weber  M. Woche  S. I. Barnes  S.‐M. Bauer  E. Beckert  W. Bittner  R. Bredthauer  T. A. Carroll  C. Denker  F. Dionies  I. DiVarano  D. Dscher  T. Fechner  D. Feuerstein  T. Granzer  T. Hahn  G. Harnisch  A. Hofmann  M. Lesser  J. Paschke  S. Pankratow  V. Plank  D. Plüschke  E. Popow  D. Sablowski  J. Storm 《Astronomische Nachrichten》2015,336(4):324-361

PEPSI is the bench‐mounted, two‐arm, fibre‐fed and stabilized Potsdam Echelle Polarimetric and Spectroscopic Instrument for the 2×8.4 m Large Binocular Telescope (LBT). Three spectral resolutions of either 43 000, 120 000 or 270 000 can cover the entire optical/red wavelength range from 383 to 907 nm in three exposures. Two 10.3k×10.3k CCDs with 9‐µm pixels and peak quantum efficiencies of 94–96 % record a total of 92 échelle orders. We introduce a new variant of a wave‐guide image slicer with 3, 5, and 7 slices and peak efficiencies between 92–96 %. A total of six cross dispersers cover the six wavelength settings of the spectrograph, two of them always simultaneously. These are made of a VPH‐grating sandwiched by two prisms. The peak efficiency of the system, including the telescope, is 15 % at 650 nm, and still 11 % and 10 % at 390 nm and 900 nm, respectively. In combination with the 110 m² light‐collecting capability of the LBT, we expect a limiting magnitude of ≈20th mag in V in the low‐resolution mode. The R = 120 000 mode can also be used with two, dual‐beam Stokes IQUV polarimeters. The 270 000‐mode is made possible with the 7‐slice image slicer and a 100‐µm fibre through a projected sky aperture of 0.74″, comparable to the median seeing of the LBT site. The 43 000‐mode with 12‐pixel sampling per resolution element is our bad seeing or faint‐object mode. Any of the three resolution modes can either be used with sky fibers for simultaneous sky exposures or with light from a stabilized Fabry‐Pérot étalon for ultra‐precise radial velocities. CCD‐image processing is performed with the dedicated data‐reduction and analysis package PEPSI‐S4S. Its full error propagation through all image‐processing steps allows an adaptive selection of parameters by using statistical inferences and robust estimators. A solar feed makes use of PEPSI during day time and a 500‐m feed from the 1.8 m VATT can be used when the LBT is busy otherwise. In this paper, we present the basic instrument design, its realization, and its characteristics. Some pre‐commissioning first‐light spectra shall demonstrate the basic functionality. (© 2015 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

Composite spectra Paper 15: HD 216572, a triple system containing a short-period, double-lined secondary     

R. E. M. Griffin †  R. F. Griffin † 《Monthly notices of the Royal Astronomical Society》2009,394(3):1393-1408

We analyse 81 optical spectra of the composite-spectrum binary HD 216572, and show that the primary is a cool giant of type G8 III while the secondary is a double-lined binary consisting of two nearly identical B9 dwarfs in a 1.18-d orbit. The inner system undergoes partial eclipses, whose photometry we model to derive the physical parameters of both secondary stars. The outer system does not eclipse. We isolate the combined spectrum of the secondary by spectral subtraction, and from 48 separate radial-velocity measurements of both secondary components we obtain a triple-lined orbit solution from which we determine the individual masses of all three stars and the inclinations of both the inner and the outer orbits. The period of the outer system is 55 d, which is surprisingly short for a giant star, and our detection of small but non-negligible amounts of variable chromospheric emission in the Ca  ii K line is not unlike that detected in other systems with comparably short periods. The secondary components are in a circular orbit and are rotating at about  95 ± 10 km s⁻¹  ; although their surface-to-surface separation is only  4 R_⊙  the stars are not noticeably distorted geometrically by such close proximity. All three stars appear to be in synchronous rotation in their respective orbits. We derive fairly accurate Hertzsprung–Russell diagram positions for all three stars and compare them to evolutionary tracks calculated for the respective stellar masses, but cannot reconcile the age of the cool giant with that of the B stars.  相似文献   

exofit: orbital parameters of extrasolar planets from radial velocities     

Sreekumar T. Balan  Ofer Lahav 《Monthly notices of the Royal Astronomical Society》2009,394(4):1936-1944

Retrieval of orbital parameters of extrasolar planets poses considerable statistical challenges. Due to sparse sampling, measurement errors, parameters degeneracy and modelling limitations, there are no unique values of basic parameters, such as period and eccentricity. Here, we estimate the orbital parameters from radial velocity data in a Bayesian framework by utilizing Markov Chain Monte Carlo (MCMC) simulations with the Metropolis–Hastings algorithm. We follow a methodology recently proposed by Gregory and Ford. Our implementation of MCMC is based on the object-oriented approach outlined by Graves. We make our resulting code, exofit , publicly available with this paper. It can search for either one or two planets as illustrated on mock data. As an example we re-analysed the orbital solution of companions to HD 187085 and HD 159868 from the published radial velocity data. We confirm the degeneracy reported for orbital parameters of the companion to HD 187085, and show that a low-eccentricity orbit is more probable for this planet. For HD 159868, we obtained slightly different orbital solution and a relatively high 'noise' factor indicating the presence of an unaccounted signal in the radial velocity data. exofit is designed in such a way that it can be extended for a variety of probability models, including different Bayesian priors.  相似文献