arXiv subjects

Yi-Ping Qin

Publications and source records attributed to Yi-Ping Qin.

33 records · Page 2Linked to original sources

arXiv2004

Relationship between different channel light curves of gamma-ray burst pulses shown in aspects other than the pulse width

In this paper, we employ the peak count rate{\bf \}$C_p$ and the total count $C_{total}$ of light curves to study in the corresponding aspects the relationship between different channel light curves. To make a direct comparison between count rates of different channel light curves we introduce a plot of $C(τ)$ versus $C_H(τ)$, where $C(τ)$ is the count rate of a channel and $C_H(τ)$ is the count rate of a definite cannel, channel H (see the text). According to the plot we define $ΔC_{\max}$ as the maximum deviation of the two count rate values of $C(τ)$ associated with a same count rate value of $% C_H(τ)$ and define $ΔS$ as the area confined by the close curve of $C(τ)$ in the plot to measure the difference of the rising and decaying portions of a light curve relative to the count rate of channel H. Under the assumption that some GRBs observed are in the stage of fireballs which expand relativistically, predictions on the relationships between the four quantities{\bf (}$C_p$, $C_{total}$, $ΔC_{\max}$, and $ΔS$) and energy within a wide band, calculated with different rest frame radiation forms and two typical Lorentz factors ($Γ=20$ and 200), are made and presented, which would make the test of our model with the coming Swift data easier. Interpretations to the relationships within the mechanism of fireballs are also presented.

astro-ph↗

arXiv2004

Characteristics of profiles of gamma-ray burst pulses associated with the Doppler effect of fireballs

In this paper, we derive in a much detail the formula of count rates, in terms of the integral of time, of gamma-ray bursts in the framework of fireballs, where the Doppler effect of the expanding fireball surface is the key factor to be concerned. Effects arising from the limit of the time delay due to the limited regions of the emitting areas in the fireball surface and other factors are investigated. Our analysis shows that the formula of the count rate of fireballs can be expressed as a function of $τ$ which is the observation time scale relative to the dynamical time scale of the fireball. The profile of light curves of fireballs depends only on the relative time scale, entirely independent of the real time scale and the real size of the objects. It displays in detail how a cutoff tail, or a turn over, feature (called a cutoff tail problem) in the decay phase of a light curve can be formed. This feature is a consequence of a hot spot in the fireball surface, moving towards the observer, and was observed in a few cases previously. By performing fits to the count rate light curves of six sample sources, we show how to obtain some physical parameters from the observed profile of the count rate of GRBs. In addition, the analysis reveals that the Doppler effect of fireballs could lead to a power law relationship between the $FWHM$ of pulses and energy, which were observed previously by many authors.

astro-ph↗

arXiv2004

Distribution of the extensive Doppler redshift of quasars

We make an analysis of the distribution of the extensive Doppler redshift defined as $\widetilde{z}_{Dopp}=(z_{abs}-z_{em})/(1+z_{em})$ with a sample of 1317 absorption redshifts available from 401 quasars. The analysis reveals a bi-peak structure in the distribution, with one component located at $\widetilde{z}_{Dopp}\simeq 0.00$ and the other at $\widetilde{z}% _{Dopp}\simeq -0.01$. A study of some possible causes suggests that the structure can be well interpreted: while the absorbers inside the same cluster as the quasar concerned could contribute to the first component and the less populated space between clusters could explain the gap between the two peaks, the typical distance between clusters could account for the second component. If the bi-peak structure is true, which needs to be confirmed by complete samples, one would be able to obtain some useful cosmological information.

astro-ph↗

arXiv2004

Doppler effect of gamma-ray bursts in the fireball framework

The influence of the Doppler effect in the fireball framework on the spectrum of gamma-ray bursts is investigated. The study shows that the shape of the expected spectrum of an expanding fireball remains almost the same as that of the corresponding rest frame spectrum for constant radiations of the bremsstrahlung, Comptonized, and synchrotron mechanisms as well as for that of the GRB model. The peak flux spectrum and the peak frequency are obviously correlated. When the value of the Lorentz factor becomes 10 times larger, the flux of fireballs would be several orders of magnitude larger. The expansion speed of fireballs is a fundamental factor of the enhancement of the flux of gamma-ray bursts.

astro-ph↗

arXiv2004

Emission and absorption lines of gamma-ray bursts affected by the relativistic motion of fireball ejecta

We display by numerical calculation how rest frame spectral lines appear in the observed spectrum of gamma-ray bursts due to the Doppler effect in the fireball framework. The analysis shows that: a) in the spectrum of a relativistically expanding fireball, all rest frame lines would shift to higher energy bands and would be significantly smoothed; b) rest frame weak narrow emission lines as well as narrow absorption lines and absorption line forests would be smoothed and would hardly be detectable; c) the features of rest frame broad emission lines as well as both strong and weak broad absorption lines would remain almost unchanged and therefore would be easier to detect; d) deep gaps caused by rest frame broad absorption lines would be significantly filled; e) a rest frame emission line forest would form a single broad line feature; f) the observed relative width of the rest frame very narrow line would approach $ 0.162$; g) when the Lorentz factor $Γ$ is large enough, the observed line frequency $ν_{line}$ and the rest frame line frequency $ν_{0,line} $ would be related by $ν_{line}\approx 2Γν_{0,line}$. We also investigate the effect of time dependence of the line intensity and the effect of variation of $Γ$. We find that the feature of rest frame dimming narrow emission lines would disappear when $Γ$ is very large. The form of emission lines would be sharp on both edges when $Γ$ varies with time. This phenomenon depends not only on the initial Lorentz factor but also on the observation time.

astro-ph↗

arXiv2002

Statistical Shapes of the Highest Pulses in Gamma--Ray Bursts

The statistical shapes of the highest pulse have been studied by aligned method. A wavelet package analysis technique and a developed pulse--finding algorithm have been applied to select the highest pulse from burst profiles observed by BATSE on board CGRO from 1991 April 21 to 1999 January 26. The results of this work show that the statistical shapes of the highest pulses are related to energy: the higher the energy, the narrower the pulse. However, the characteristic structures of the pulses have nothing to do with energy, which strongly supports the previous conclusion that the temporal profiles in different channels are self--similar. The characteristic structures of the pulses can be well described by a model proposed by Norris et al. (1996). The fitting parameters are: $t_r$=0.12, $t_d$=0.16, $\upsilon =1.09$, the ratio of $t_r$ to $t_d$ for the pulse is 0.75. The result leads to our conjecture that the mechanisms of bursts in different gamma-ray bands might be the same. The shock, either an internal or an external one, producing the pulse, might emit photons over the four energy channels in the same way.

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arXiv2002

Twin jets as a potential distance detector

A preview study of using observational data of proper motions and Doppler shifted velocities of twin-jets to determine the distance of sources inside and outside our galaxy is made. We investigate the feasibility of this method by studying the uncertainty of the distance caused by the uncertainties of the measured quantities. It shows that, when the motion of components of the jet is relativistic, then the uncertainty of the distance is within the same order of the uncertainties of the measured values of proper motions and Doppler shifted velocities. In particular, when assuming the pattern speed equals the flow speed in the jet, for 10% uncertainties of the measured quantities, the uncertainty of the distance caused by them would be well within 13%. With current technique, this method is realizable. For the convenience of choosing sources to observe, some sources as potential targets are also listed in this paper.

astro-ph↗

arXiv2000

Formulas for direct determination of real speed in Galactic superluminal sources

In this paper we show explicit and direct relations between the expected quantities and the observed quantities for the components of Galactic superluminal sources. Basic formulas for calculating the real speed and the angle to the line of sight of the components from the data of proper motions and the distance of the source are presented. We point out that the real speed and the angle to the line of sight of components can be uniquely and directly determined from the observed values of the proper motions and the distance of the source. It is not necessary to calculate an intermediate quantity first and then using the resulted value to calculate the two required quantities. The process of the calculation is simple, and in this way, some extra uncertainties are avoided.

astro-ph↗

arXiv2000

Distinguishing RBL-like objects and XBL-like objects with the peak emission frequency of the overall energy spectrum

We investigate quantitatively how the peak emission frequency of the overall energy spectrum is at work in distinguishing RBL-like and XBL-like objects. We employ the sample of Giommi et al. (1995) to study the distribution of BL Lacertae objects with various locations of the cutoff of the overall energy spectrum. We find that the sources with the cutoff located at lower frequency are indeed sited in the RBL region of the $α_{ro}-α_{ox}$ plane, while those with the cutoff located at higher frequency are distributed in the XBL region. For a more quantitative study, we employ the BL Lacertae samples presented by Sambruna et al. (1996), where, the peak emission frequency, $ν_p$, of each source is estimated by fitting the data with a parabolic function. In the plot of $α_{rx}-\log ν_p$ we find that, in the four different regions divided by the $α_{rx}=0.75$ line and the $\log ν_p=14.7$ line, all the RBL-like objects are inside the upper left region, while most XBL-like objects are within the lower right region. A few sources are located in the lower left region. No sources are in the upper right region. This result is rather quantitative. It provides an evidence supporting what Giommi et al. (1995) suggested: RBL-like and XBL-like objects can be distinguished by the difference of the peak emission frequency of the overall energy spectrum.

astro-ph↗

arXiv2000

A simple method of determining the Hubble constant

Bidirectional relativistic proper motions of radio components of nearby extragalactic sources give a strong constraint on the determination of the Hubble constant $H_0$. Under the assumption that the real velocity of radio components of extragalactic sources is not less than that of Galactic sources, the value of $H_0$ can be estimated at a high level of accuracy. The assumption is reasonable due to the general belief that the activity in the core of galaxies must be more powerful than that of stars. This method is simple and with only one uncertainty --- the real velocity of components. This uncertainty is related to the value of the real velocity of componenets of Galactic sources and the latter is always well-determined (note that the determination is independent of $H_0$ and the distance of Galactic sources can be directly measured at a rather high level of accuracy). Hopefully the method will play an important role in future research to fix the value of $H_0$. With the data of the three sources available so far and the assumption that the real velocity of componenets of at least one of the sources is not less than a known velocity of componenets of a Galactic source, the constant is estimated to be within $27.08kms^{-1}Mpc^{-1} < H_0 \leq 53.15kms^{-1}Mpc^{-1}$ with this method.

astro-ph↗

arXiv2000

Correlations between various hardness ratios of gamma-ray bursts

We study correlations between various hardness ratios of gamma-ray bursts (GRBs) and investigate if there are any differences between the two classes of the objects in the distributions of the ratios. The results suggest that, statistically, the slope of the higher part of the spectrum of the long duration bursts has nothing to do with that of the lower part; emissions at higher energy bands from the bursts of both short and long duration classes must be significantly different for different sources, while radiations at lower energy bands of the objects are relatively similar; the spectrum of the short duration bursts must be harder than that of the long duration bursts, confirming what the well-known hardness-duration correlation reveals; the profiles of the spectra between the long duration bursts must be more similar than that between the short duration bursts. The long duration bursts would share more common properties than the short duration bursts. A possible interpretation is proposed with the concept of the Doppler boosting in the relativistic beaming model in AGNs.

astro-ph↗

arXiv2000

The hardness-duration correlation in the two classes of gamma-ray bursts

The well-known hardness-duration correlation of gamma-ray bursts (GRBs) is investigated with the data of the 4B catalog. We find that, while the hardness ratio and the duration are obviously correlated for the entire set of the 4B catalog, they are not at all correlated for the two subsets divided at the duration of 2 seconds. However, for other subsets with comparable sizes, the two quantities are significantly correlated. The following conclusions are then reached: (1) the existence of two classes of GRBs is confirmed; (2) the hardness ratio and the duration are not at all correlated for any of the two classes; (3) different classes of GRBs have different distributions of the hardness ratio and the duration and it is this difference that causes the correlation between the two quantities for the entire set of the bursts.

astro-ph↗

arXiv2000

An Accelerated Expansion Model in the Absence of the Cosmological Constant

Based on some observations, the apparent energy, associated with gravity, of vacuums is defined, with that of normal vacuums to be zero and that of the vacuums losing some energy to be negative. An important application of the energy is its contribution to Einstein's equation. A cosmological model, accounting for recent observations of the accelerated expansion of the universe, in the absence of the cosmological constant, can be well constructed. In a certain case, the expansion of the universe would be decelerated at its early epoch and accelerated at its late epoch. The curvature of the universe would depend on the ratio of matter energy to total energy. The missing mass problem does no longer exist in this model. Most negative apparent energy vacuums might be contained in voids, then the spacetime of galaxy clusters or that of the solar system would not be significantly affected by this kind of energy.

gr-qc↗

arXiv2000

Evidence consistent with the cosmological interpretation of quasar redshifts

In this letter, the old issue of whether redshifts of quasars are of cosmological origin is investigated. We make a plot of absorption redshifts versus emission redshifts for quasars with large amounts of data. Our study shows that, almost all absorption redshifts are smaller than the corresponding emission redshifts. The relation between the absorption and emission redshifts predicted by current cosmological models is well obeyed. The result confirms that redshifts of quasars are indeed distance indicators. It might be the most obvious evidence found so far to be consistent with the cosmological interpretation of quasar redshifts.

astro-ph↗

arXiv2000

Causal relation between regions I and IV of the Kruskal extension

By extending the exterior Schwarzschild spacetime in two opposite directions with the Kruskal method, we get an extension which has the same T-X spacetime diagram as has the conventional Kruskal extension, while allowing its regions I and IV to correspond to different directions of the original spacetime. We further extend the exterior Schwarzschild spacetime in all directions and get a 4-dimensional form of the Kruskal extension. The new form of extension includes the conventional one as a part of itself. From the point of view of the 4-dimensional form, region IV of the conventional extension does not belong to another universe but is a portion of the same exterior Schwarzschild spacetime that contains region I. The two regions are causally related: particles can move from one to the other.

gr-qc↗