共查询到20条相似文献，搜索用时 453 毫秒
1.
利用线性状态空间模型（Ｌｉｎｅａｒ Ｓｔａｔｅ Ｓｐａｃｅ Ｍｏｄｅｌ－ＬＳＳＭ）,将 Ｃｙｇ Ｘ－１的功率谱分解为ＬＳＳＭ产生的模型功率谱和剩余功率谱两部分．集中分析剩余功率谱,结果显示, Ｃｙｇ Ｘ－１在低／硬态、转换态和高／软态三种状态的剩余功率谱有着不同的结构特征．其中高／软态和低／硬态的剩余功率谱存在一个宽峰结构,中心频率分别为～ ８ Ｈｚ和～ ５ Ｈｚ,低／硬态的剩余功率诺在～ ０．０７ Ｈｚ达到极大;转换态的剩余功率谱有双峰结构,其中心频率分别在～０．５—４Ｈｚ和～５—１１Ｈｚ,与我们以前分析的 ＱＰＯ的中心频率很接近,说明 ＱＰＯ与线性状态空间所要求的自回归模型可能属于不同的物理过程．与总功率谱比较,剩余功率谱对谱的变化部分（例如ＱＰＯ、截断频率等）更为敏感,本文对剩余功率谱中谱峰变化的原因做了初步的探讨． 相似文献
2.
针对天文观测数据不等间隔的特点,利用Jurkevich方法对黑洞候选体X射线双星Cyg X-1近16年的Rossi X-ray Timing Explorer(RXTE)All-Sky Monitor(ASM)数据进行了频谱分析,并结合Kidger周期存在可信度的判据,发现Cyg X-1存在363±11.5 d的光变周期,但没有发现420 d的光变周期,而且150 d的光变周期可能仅仅是51±1.4 d光变周期的观测表象。 相似文献
3.
运用自回归功率普研究Ｃｙｇ Ｘ－１ Ｘ辐射的频谱特征,结果显示Ｃｙｇ Ｘ－１转换态和高／软态时变频谱的连续成分,可以统一由有截断的幂律的成分描述,转换态存在小地３ＨＺ的宽峰结构及准周期振荡（ＱＰＯ）成分（４－１２ＨＺ）,而高／软态完全可由截断幂律普描述,不存在显著的ＱＰＯ。截断频率在各态相相当,在不同态的演化与平流为主的吸积流模型（ＡＤＡＦ（预期的情形一致。本文结果表明,自回归功率 研究Ｘ射线双 相似文献
4.
CygX-1高能辐射的时变特征可以通过短暴(shot)的性质反映．因此CygX-1的短暴性质，特别是处于低态时的性质曾被广泛研究,利用直接叠加短暴和自相关函数，对CygX-1高态时短暴的性质进行了研究．结果表明，当CygX-1处于高态时，其短暴的结构类似于低态时所具有的性质，短暴的半高宽随能量的增加按指数下降．此结果和康普顿化模型不一致．另外，短暴的能谱演化及结构的非对称性可以解释CygX-1中的时延现象． 相似文献
5.
本文在对NML Cyg OH 1612MHz脉塞辐射的Masheder等长基线干涉仪观测结果的分析中,引进了红移分量和蓝移分量在不同拱星包层壳层中发生的新观念,得到了NML Cyg拱星包层的球形外流场模型.并讨论了质量流失、相干长度和抽运机制等问题,结论与观测符合.这在红超巨星脉塞源长基线干涉仪观测结果的分析中,还是首次获得成功.由本文的结论可看到,SiO非脉塞辐射(v=0、J=2-1)是红外星视向速度和包层流场的好的指示器. 相似文献
6.
We have calculated the spectrum of Cyg X-1 under the assumption that the radiation orginates in a disk around a 11M
black-hole. Supersonic turbulence prevails in the outer parts of the disk and electron-electron bremsstrahlung appears to be resonsible for the maintenance of the temperature at a level less than 1010 K near the inner edge of the disk. The theoretical spectrum gives the best fit with the observations if the Reynolds number is about 1200. 相似文献
7.
High-resolution optical spectroscopy of the V2324 Cyg variable star associated with the IR source IRAS 20572+4919 is performed for the first time. More than 200 absorption features (mostly Fe II, Ti II, Cr II, Y II, Ba II, and Y II) are identified in the wavelength interval from 4549 to 7880 Å. The spectral type and rotation velocity of the star are found to be F0 III and V sin i = 69 km/s, respectively. Neutral-hydrogen and NaI D lines have complex P Cyg-type profiles. Neither systematic trend of radial velocity Vr with line depth Ro nor temporal variability of Vr have been found. We found that the value for the average heliocentric radial velocity is Vr = ?16.8 ± 0.6 km/s. The radial velocities inferred from the cores of the absorption components of the Hβ and NaI wind lines vary from ?140 to ?225 km/s (and the expansion velocities of the corresponding layers, from about 120 to 210 km/s). The maximum expansion velocity is found for the blue component of the split Hα absorption: 450 km/s for December 12, 1995. The method of model atmospheres is used to determine the following parameters of the star: effective temperature T eff = 7500 K, surface gravity log g = 2.0, microturbulence velocity ξ t = 6.0 km/s, and metallicity, which is equal to the solar value. The main peculiarity of the chemical composition of the star is the overabundance of lithium and sodium. The results cast some doubt on the classification of V2324 Cyg as a post-AGB star. 相似文献
8.
Spectrophotometric observations in optical region ( 38008000 Å) on the symbiotic object V 1329 Cyg (HBV 475) were carried out with the 122 cm telescope of the Astrophysical Observatory of Asiago in 1979 and 1980. Significant changes of intensity of emission lines with a time-scale of a few weeks were observed. The results of these observations suggest that probably V 1329 Cyg is a Nova-like object with recurrent outbursts at intervals of about 950 days. The properties of this object seem to agree with those of a white dwarf which is accreting mass rapidly. 相似文献
9.
Z. B. Li L. M. Song J. L. Qu Y. J. Lei J. Y. Nie C. M. Zhang 《Astrophysics and Space Science》2012,341(2):383-393
In this paper, the rms-flux (root mean square-flux) relation along the Z-track of the bright Z-Source Cyg X-2 is analyzed using the observational data of Rossi X-ray Timing Explorer (RXTE). Three types of rms-flux relations, i.e. positive, negative, and ‘arch’-like correlations are found in different branches. The rms is positively correlated with flux in normal branch (NB), but anti-correlated in the vertical horizontal branch (VHB). The rms–flux relation shows an ‘arch’-like shape in the horizontal branch (HB). We also try to explain this phenomenon using existing models. 相似文献
10.
11.
Preliminary results from a search for emission stars in the neighborhood of Cyg OB7 are reported. A new region of size 14×14
arc min lies 12 arc min to the south of HH 448. 17 new objects have been found, of which one is related to a nebula with an
interesting shape and, apparently, the characteristics of a cometary nebula. Inside the nebula there are 4 faint, compact
formations with very high proper motions. The spectrum of a star shows that it is of spectral class K9-M0 and is a T Tau type
star at a distance of 220 pc. Most of the discovered stars with a strong or intermediate Ha emission line intensity are presumably
also T Tau stars. This region appears to be a continuation of the T association around HH 448. 相似文献
12.
本文发表了对天鹅座32食双星1981年食期间及1982年食外期间,在波段范围λλ3520—4348A及λλ5110—6600A的光谱观测结果.分析了Call K线等值宽度随位相的变化,推算了K型超巨星色球大气的密度分布规律;测定了K星的视向速度;认证及测定了光谱中的发射线和呈P Cyg轮廓的谱线,并估算了K型超巨星的质量损失率. 相似文献
13.
E. S. Dmitrienko 《Astrophysics》1996,39(2):112-114
UBVRI observations of the eclipsing symbiotic star CI Cyg made during 1991–1995 are analyzed, the results of which indicate that the system is in the same quiescent state as during 1985–1990. Variations in the "extra-eclipse" color index U-B with an amplitude of about 0m.3–0m.4 and a characteristic time of about 9–10 yr have been detected for the first time. A more thorough analysis of all available data in the UBVRI bands of the spectrum will be required to investigate the existence of possible long-period variations in the other color indices and brightness of the system.Translated fromAstrofizika, Vol. 39, No. 2, pp. 211–216, April–June, 1996. 相似文献
14.
15.
利用Rossi X-ray Timing Explorer(RXTE)卫星从1996年1月到2005年5月的公共资料,研究了黑洞候选体X射线双星Cyg X-1光变曲线的周期性,并且发现了一些有趣的周期特性(T=1．0±0．2天和T=18．0±3．0天)．在硬态时,T=1．0±0．2天和T=18．0±3．0天的周期特性同时出现在它的光变曲线之中,但在软态时仅有T=1．0±0．2天的周期出现．采用一种新的方法(即微分法),同时为了检验微分法的正确性,还利用传统的方法(即快速傅立叶变换和叠加法)分析了相同的资料,并得到了与微分法相同的结果．另外也对Cyg X-1的轨道周期进行了研究,结果发现T=5．6天的轨道周期不仅出现在硬态,同时也出现在软态,只是在硬态时比在软态时明显． 相似文献
16.
17.
本文详细讨论了X射线双星Cyg X-3 的X光子场对γ射线的吸收效应.计算结果表明:当Cyg x-3 的X光子发射场处于高态时,从致密中子星附近发射的能量为10~2—10~4MeV的γ射线约有60％被其吸收,吸收过程产生的正负电子的逆Compton 散射会使出射能量10—70MeV的γ射线强度平均增加约50％.计算的γ射线能谱与实验观测结果基本相符. 相似文献
18.
We present the results of our infrared observations of WR 140 (=V1687 Cyg) in 2001–2010. Analysis of the observations has
shown that the J brightness at maximum increased near the periastron by about 0
m
.3; the M brightness increased by ∼2
m
in less than 50 days. The minimum J brightness and the minimum L and M brightnesses were observed 550–600 and 1300–1400 days after the maximum, respectively. The JHKLM brightness minimum was observed in the range of orbital phases 0.7–0.9. The parameters of the primary O5 component of the
binary have been estimated to be the following: R(O5) ≈ 24.7R
⊙, L(O5) ≈ 8 × 105
L
⊙, and M
bol(O5) ≈ −10
m
. At the infrared brightness minimum, T
g ∼ 820–880 K, R
g ≈ 2.6 × 105
R
⊙, the optical depth of the shell at 3.5 μm is ∼5.3 × 10−6, and its mass is ≈1.4 × 10−8
M
⊙. At the maximum, the corresponding parameters are ∼1300 K, 8.6 × 104
R
⊙, ∼2 × 10−4, and ∼6 × 10−8
M
⊙; the mean rate of dust inflow (condensation) into the dust structure is ∼3.3 × 10−8
M
⊙ yr−1. The mean escape velocity of the shell from the heating source is ∼103 km s−1 and the mean dispersal rate of the shell is ∼1.1 × 10−8
M
⊙ yr−1. 相似文献
19.
利用离散傅里叶分析法,基于RXTE (Rossi X-ray Timing Explorer)/ASM(All-Sky Monitor,1.5～12 keV)观测数据,对黑洞候选体X射线双星Cyg X-1硬度比HR(5～12 keV/3～5 keV)(简写HR)的时变特性进行了分析,结果表明黑洞候选体X射线双星Cyg X-1硬度比HR存在明显的周期特性:(1)混合态(硬态+软态,本文指MJD=50087～55841期间所有的观测数据)时,HR存在T≈5.6 d、40.0 d、78.4 d、173.8 d以及400/800 d的时变周期; (2)硬态时, HR存在T≈5.6 d、33.7/67.6 d、45.3 d和165.3 d的周期特性; (3)软态时,HR出现了T≈38.5 d、48.1 d和128.3 d的周期性变化.并利用粘滞理论和Zdziarski吸积盘模型讨论了以上周期特性的物理机制. 相似文献
20.
《天文和天体物理学研究(英文版)》2020,(7)
New V-band CCD observations of variable star V2455 Cyg were performed during two nights in September 2017. According to all times of maximum light and new maxima, the O-C curve was analyzed.The period changes of V2455 Cyg were investigated and the rate of increasing period was obtained to be(1/P) d P/dt = 1.99 × 10~(-7) yr~(-1). Frequency analysis indicated that V2455 Cyg pulsates with the radial p mode and the fundamental frequency is 10.61574 d-1. Physical parameters of V2455 Cyg at mean temperature were determined(e.g., R = 2.52 R_⊙and M = 1.92 M_⊙). The position of this star in the H-R diagram confirms that V2455 Cyg is a high amplitude δ Scuti star. 相似文献