IRTF observations of white dwarfs with possible near-infrared excess     

J. Farihi 《Monthly notices of the Royal Astronomical Society》2009,398(4):2091-2109

Near-infrared photometry and spectroscopy are obtained for a heterogeneous sample of nearby white dwarfs with possible excess flux as identified primarily in the Two Micron All Sky Survey. Among the sample of 43 stars are a number of white dwarfs that are either metal-rich, magnetic or binary suspects. With a few notable exceptions in four (or possibly five) distinct categories, the newly obtained JHK photometric data fail to corroborate the putative excesses, with  〈 K _IRTF− K _2MASS〉=+0.31  mag. Where available, Galaxy Evolution Explorer photometric data are used to better constrain the overall spectral energy distribution of the white dwarfs, enabling any excess near-infrared flux to stand out more readily against the expected stellar photosphere.
With superior data, a near-infrared photometric excess is confirmed at three metal-rich white dwarfs and ruled out at nine others. Several new binaries are confirmed or suggested; five white dwarf–red dwarf pairs and five double degenerates. Four apparently single magnetic white dwarfs – two DA and two DQp – display modest to strong near-infrared excess (relative to non-magnetic models), which may be better described as two effective temperatures owing to a redistribution of energy in highly magnetic or peculiar atmospheres.  相似文献   

Is there evidence for field restructuring or decay in accreting magnetic white dwarfs?     

C. M. Zhang  D. T. Wickramasinghe  Lilia Ferrario 《Monthly notices of the Royal Astronomical Society》2009,397(4):2208-2215

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江西早稻穗瘟发生的气象条件监测预警方法   总被引：2，自引：0，他引：2  

郭瑞鸽  杜筱玲  刘文英  胡菊芳 《气象与减灾研究》2008,31(3):48-51

稻瘟病的发生受气象环境的影响显著,因此根据代表江西不同区域站点的早稻穗瘟发生情况,选取病害同期气象资料,从稻瘟病病菌致病所要求的气象条件出发,利用温度、湿度、降水、日照等气象因子构建天气促病指数,并将之划分为有利、较有利、不利3个级别来反映气象条件对早稻穗瘟发生的适宜程度。对比分析检验与监测试用情况的结果表明,模型对病害发生气象适宜程度的指示性较好。  相似文献   

Accreting white dwarfs as supersoft X‐ray sources     

M. Kato 《Astronomische Nachrichten》2010,331(2):140-145

I review various phenomena associated with mass‐accreting white dwarfs (WDs) in the view of supersoft X‐ray sources. When the mass‐accretion rate is low (Ṁ_acc < a few × 10^–7 M⊙yr^–1), hydrogen nuclear burning is unstable and nova outbursts occur. A nova is a transient supersoft X‐ray source (SSS) in its later phase which timescale depends strongly on the WD mass. The X‐ray turn on/off time is a good indicator of the WD mass. At an intermediate mass‐accretion rate an accreting WD becomes a persistent SSS with steady hydrogen burning. For a higher mass‐accretion rate, the WD undergoes “accretion wind evolution” in which the WD accretes matter from the equatorial plane and loses mass by optically thick winds from the other directions. Two SSS, namely RX J0513‐6951 and V Sge, are corresponding objects to this accretion wind evolution. We can specify mass increasing WDs from light‐curve analysis based on the optically thick wind theory using multiwavelength observational data including optical, IR, and supersoft X‐rays. Mass estimates of individual objects give important information for the binary evolution scenario of type Ia supernovae (© 2010 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

X‐ray energy spectra of CAL87     

K. Ebisawa  T. Rauch  D. Takei 《Astronomische Nachrichten》2010,331(2):152-155

We present X‐ray spectral analysis of the super‐soft source CAL87 using ASCA, Chandra, XMM‐Newton observations. Early ASCA CCD spectrum reported a strong oxygen absorption edge, which is considered to originate in the an optically thick white‐dwarf atmosphere. On the other hand, contemporaneous grating observations by Chandra and XMM‐Newton indicate emission line dominated spectra, which obviously indicate the optically thin origin. Fitting all the available CCD (ASCA and XMM‐Newton) and grating spectra (XMM‐Newton and Chandra) simultaneously, we show that the CAL87 X‐ray energy spectrum is in fact composed of both an optically thick component with deep absorption edges and an optically thin component with numerous emission lines. The current result supports the standard SSS model that the primary source of X‐ray emission is nuclear burning in the white dwarf atmosphere, surrounded by a highly photoionised, optically thin corona (© 2010 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

Swift observations of CSS081007:030559+054715     

A.P. Beardmore  J.P. Osborne  K.L. Page  G. Schwarz  S. Starrfield  P. Hakala  J.‐U. Ness  S. Balman  R.M. Wagner 《Astronomische Nachrichten》2010,331(2):156-159

CSS081007:030559+054715 was discovered by the Catalina Real‐time Transient Survey. Optical spectroscopy revealed a multi‐peaked Hα emission line profile with radial velocities exceeding 1500 km/s, as well as strong Ne emission, suggestive of a neon nova. We monitored the source extensively with the Swift satellite, obtaining a unique dataset spanning 270 days in the soft X‐ray and UV bands. The data reveal a soft, blackbody‐like spectrum with a temperature around 55 eV (though dependent on the modelling), variable X‐ray and UV light curves with a 1.77 day period in both the X‐ray and UV bands, a longer timescale modulation of ∼ 50 days, followed by a slowly declining trend in the soft X‐ray and UV flux. We highlight the Swift observations and their implications for the SSS nature of this object (© 2010 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

On the DB gap of white dwarf evolution:effects of hydrogen mass fraction and convective overshooting     

Jie Su  Yan Li National Astronomical Observatories/Yunnan Observatory  Chinese Academy of Sciences  Kunming  China  Graduate University of Chinese Academy of Sciences  Beijing 《中国天文和天体物理学报》2010,10(3)

We investigate the spectral evolution of white dwarfs by considering the effects of hydrogen mass in the atmosphere and convective overshooting above the convection zone.Our numerical results show that white dwarfs with MH～10-16M⊙ show the DA spectral type between 46000■Teff■26000K and the DO or DB spectral type may appear on either side of this temperature range.White dwarfs with10-15M⊙ appear as DA stars until they cool to Teff～31000K;from then on they will evolve into DB white dwarfs as a result of conve...  相似文献   

The white dwarf luminosity function – II. The effect of the measurement errors and other biases     

Santiago Torres  Enrique García-Berro  Jordi Isern 《Monthly notices of the Royal Astronomical Society》2007,378(4):1461-1470

The disc white dwarf luminosity function is an important tool for studying the solar neighbourhood, since it allows the determination of several Galactic parameters, the most important one being the age of the Galactic disc. However, only the     method has been employed so far for observationally determining the white dwarf luminosity function, whereas for other kind of luminosity functions several other methods have been frequently used. Moreover, the procedures to determine the white dwarf luminosity function are not free of biases. These biases have two different origins: they can either be of statistical nature or a consequence of the measurement errors. In a previous paper we carried out an in-depth study of the first category of biases for several luminosity function estimators. In this paper we focus on the biases introduced by the measurement errors and on the effects of the degree of contamination of the input sample used to build the disc white dwarf luminosity function by different kinematical populations. To assess the extent of these biases we use a Monte Carlo simulator to generate a controlled synthetic population and analyse the behaviour of the disc white dwarf luminosity function for several assumptions about the magnitude of the measurement errors and for several degrees of contamination, comparing the performances of the most robust luminosity function estimators under such conditions.  相似文献   

A Simplified Technique for Simulating Wide-band Strong Ground Motion for Two Recent Himalayan Earthquakes   总被引：1，自引：0，他引：1  

A.?JoshiEmail author 《Pure and Applied Geophysics》2004,161(8):1777-1805

A simplified technique for simulation of wide-band strong motion based on simple regression relations and Empirical Greens Function (EGF) technique by Irikura (1986) is presented in this paper. The method uses the acceleration envelope as a shaping window for a filtered white Gaussian noise, to get the synthetic accelerogram from each subfault. Correction factors for slip of large and small events and transmission factors at each boundary of different layers are included in this synthetic accelerogram. The synthetic accelerogram obtained from each subfault is used as the Greens function to get resultant records. Simulations are made for the confirmed models of the Uttarkashi and the Chamoli earthquakes at a number of stations to get wide-band strong ground motion. The comparison of synthetic with the observed records over a wide range of frequencies for two different Himalayan earthquakes establishes the efficacy of the present technique.  相似文献   

Broadband X-ray spectrum of the intermediate polar V2400 Oph     

M. G. Revnivtsev  A. A. Lutovinov  B. F. Suleimanov  S. V. Molkov  R. A. Sunyaev 《Astronomy Letters》2004,30(11):772-778

We present the results of our analysis of the observations of the intermediate polar V2400 Oph by the INTEGRAL and RXTE observatories. We reconstructed the spectrum of the source over a wide (3–100 keV) energy range. The spectrum obtained can be fitted by a computed theoretical model of the post-shock emitting region with T_max～22 keV. As a result, we estimated the mass (0.59M_⊙) and radius (8.8×10⁸ cm) of the white dwarf in the system V2400 Oph.  相似文献