• <tr id="yyy80"></tr>
  • <sup id="yyy80"></sup>
  • <tfoot id="yyy80"><noscript id="yyy80"></noscript></tfoot>
  • 99热精品在线国产_美女午夜性视频免费_国产精品国产高清国产av_av欧美777_自拍偷自拍亚洲精品老妇_亚洲熟女精品中文字幕_www日本黄色视频网_国产精品野战在线观看 ?

    Study on the X-Ray Re-brightening Signature of GRB 220117A

    2024-01-06 06:40:28LiTaoZhao
    Research in Astronomy and Astrophysics 2023年11期

    Li-Tao Zhao

    School of Mathematics and Science, Hebei GEO University, Shijiazhuang 050016, China; zhaolt@mail.bnu.edu.cn

    Abstract The Swift/XRT detected the X-ray afterglow of long burst GRB 220117A,which began to rebrighten 300 s after triggering and followed a single power-law decay segment after thousands of seconds of the orbital observation gap.This segment is different from the shallow decay segment(plateau)and flare,and may belong to a giant X-ray bump.We investigated this segment by the fall-back accretion model and found that the model can interpret this segment with reasonable parameter values.Within this physical model scenario,the fall-back accretion rate reaches a peak value ~1.70×10-5M⊙s-1 around 300 s in the central engine frame, which is compatible with the late mass supply rate of some low-metallicity massive progenitor stars.The initial black hole (BH) spin isand implies that this re-brightening signature requires a larger BH spin.The total accretion mass during the fall-back process is Macc=(3.09±0.02)×10-2M⊙.The jet energy from the fall-back accretion is(9.77±0.65)×1052 erg, with a ratio of 0.066 to the isotropic-equivalent radiation energies of the GRB prompt phase in the 1–104 keV band.The fall-back radius rp corresponding to the peak time of fall-back tp is(3.16±0.05)×1010 cm, which is consistent with the typical radius of Wolf–Rayet stars.In summary, our results provide additional support for the origin of the long burst from the core collapse of Wolf–Rayet stars,and its late central engine activity is likely due to the fall-back accretion process.

    Key words: accretion – accretion disks – black hole physics – (stars:) gamma-ray burst: general

    1.Introduction

    Gamma ray bursts (GRBs) are the brightest electromagnetic event that have occurred in the universe since the Big Bang,consisting of two emission phases: the prompt emission(with an initial prompt soft γ-ray emission) and afterglow emission(with long term broadband emission).The prompt emission is generally considered to be related to the internal dissipation of the jet, such as internal shock dissipation or magnetic dissipation.Afterglow emission is usually considered to be from external shocks (especially forward shock) generated by the interaction between jets and interstellar medium (see Zhang 2018 for a review).In general, the end of the prompt emission phase means that the cease of GRB’s central engine.However, observations from Swift satellite indicate that many GRB’s central engines have an extended activity time, mainly manifested as shallow decay segments (plateaus) (Liang et al.2007; Troja et al.2007; Tang et al.2019; Zhao et al.2019),flares (Burrows et al.2005; Zhang et al.2006; Margutti et al.2011), and giant bumps (Kumar et al.2008a; Wu et al.2013;Gao et al.2016;Chen et al.2017;Zhao et al.2020,2021)in the X-ray light curves following the prompt emission.

    The Swift/XRT detected the X-ray afterglow of long burst GRB 220117A, which began to rebrighten 300 s after triggering and suggest that this GRB has an extended central engine activity time.In addition,this signature is different from X-ray shallow decay segment (plateau) and flare, and may belong to a giant X-ray bump.Due to the absence of an“internal plateau” feature in the X-ray afterglow of GRB 220117A,its central engine may be a hyperaccreting black hole(BH) system.In this physical scenario, the internal dissipation of fall-back accretion energy can interpret the giant X-ray bump.If the fall-back accretion rate or the duration of fall-back accretion process is large enough, a giant X-ray bump that rapidly rises and decays with a form of t-5/3is expected.So far, the giant X-ray bump has been found in the X-ray afterglow of many GRBs and could be well interpreted within the fall-back accretion model(Wu et al.2013;Gao et al.2016;Chen et al.2017; Zhao et al.2021).

    In this paper,we study the X-ray re-brightening signature of GRB 220117A within the fall-back accretion model.In Section 2, we describe the observations of GRB 220117A and analyze the re-brightening signature.The fall-back accretion model is described in Section 3.In Section 4, we apply the fall-back accretion model to the re-brightening signature.The conclusion and implications of our results are discussed in Section 5.Throughout the paper, the convention Q=10nQnis adopted in c.g.s.units.

    2.GRB 220117A Observations

    Figure 1.The XRT light curve of GTB 220117A.The solid red lines are the best fits with a smooth broken power law for the X-ray re-brightening phase and its follow-up decay phase.

    The BAT triggered and located GRB 220117A at 23:58:21 UT on 2022 January 17.T90(15–350 keV) is 49.81±2.37 s.The time-averaged spectrum from T+14.79s to T+66.14s is best fitted by a single power law (SPL) function.The powerlaw index of the time-averaged spectrum is Γγ=1.8±0.18.The fluence in the 15–150 keV band is Sγ=1.6±0.2×10-6erg cm-2(Palmer et al.2022).XRT observations started at 151.9 s after the trigger.The XRT light curve is shown in Figure 1.The UVOT starts collecting data 161 s after the trigger.No source was detected by the UVOT at the X-ray afterglow position(Melandri et al.2022).Palmerio et al.(2022)observed the afterglow of GRB 220117A using the ESO VLT UT3.From the feature of Lyα trough and the Si II 1260 AA,the redshift was measured as z=4.961.

    For the re-brightening segment and follow-up segment of GRB 220117A,we adopted a smooth broken power law(BPL)function to fit it,

    where α1and α2represent the decay scope before and after the break, respectively.w describes the sharpness of break, and here we adopt w=3 as suggested by Liang et al.(2007).The fitting light curve and the best fitting parameters are shown in Figure 1.In 2019,Zhao et al.(2019)found that the decay scope of a shallow decay segment accords with normal distribution α1=0.35±0.35 based on 13 yr of Swift/XRT observation data.It can be inferred that X-ray re-brightening segment may not be a shallow decay segment.

    In addition, we also tested whether the X-ray re-brightening segment and follow-up segment belong to the flare.Yi et al.(2016) analyzed the GRBs with significant flares observed by Swift/XRT from 2005 April to 2015 March and obtained an empirical relationship:

    where Tpeakis the peak time of the fare.Tdur=Tend-Tstartis the duration of the flare,where Tstartand Tendrepresent the start time and end time of the flare, respectively.Tpeakand Tdurof each flare could be easily obtained by fitting the light curve with a smooth BPL function.We find that the duration of X-ray re-brightening segment and its follow-up decay segment deviates from the duration obtained by the empirical relationship 2σ.Compared to the typical flare, the giant X-ray bump has a relatively longer duration.Therefore, the X-ray rebrightening segment and follow-up segment may belong to a giant X-ray bump.

    3.Model Description

    In this paper,we intend to use the fall-back accretion model to interpret the X-ray re-brightening segment of GRB 220117A.The physical scenario of the fall-back accretion model is described as follows: the progenitor stars of long GRBs may be massive stars (Woosley 1993; Paczyński 1998;MacFadyen & Woosley 1999; Woosley & Bloom 2006), and generally have a core-envelope structure.At the end of the massive stars’ evolution, photodisintegration and electron capture will trigger core collapse and form a super accretion BH system.The relative jet is launched by the super accretion BH system through extracting the gravitational energy from the accreted material or the spin energy of the BH.When the relativistic jet successfully penetrates the envelope, it powers initial prompt emission and broadband afterglow emission of the GRB.During the process of jet penetration through the progenitor envelope, a part of jet energy is transferred to the envelope, which might help the supernova to explode.The bounding shock responsible for the associated supernova transfers kinetic energy to the envelope materials and a part of envelope materials would be ejected.The rest of envelope materials could fall back into around of BH and form an accretion disk(Kumar et al.2008a,2008b).The accretion disk may power a new relativistic jet through the neutrinoannihilations mechanism (Popham et al.1999; Narayan et al.2001;Di Matteo et al.2002;Janiuk et al.2004;Gu et al.2006;Chen & Beloborodov 2007; Liu et al.2007, 2015; Lei et al.2009, 2017; Xie et al.2016) or Blandford–Znajek (BZ)mechanism (Blandford & Znajek 1977; Lee et al.2000;Li 2000; Lei et al.2005, 2013).Compared with the neutrinoannihilations mechanism, the jet powered by the BZ mechanism will be cleaner and more powerful (Lei et al.2017; Xie et al.2017; Lloyd-Ronning et al.2018).Therefore, the BZ mechanism is more likely to interpret the late central engine activity of long GRBs.A part of BZ energy would eventually be injected into the afterglow blast wave.If the injected energy is comparable to or even larger than the blast wave kinetic energy, it will generate some detectable signature such as a plateau in the X-ray afterglow (Zhao et al.2020).In addition,the rest energy would undergo the internal dissipation process,which may generate the observed giant X-ray bump.

    The evolution of the fall-back rate of progenitor envelope material can be described by a smooth BPL function as(Chevalier 1989; MacFadyen et al.2001; Zhang et al.2008;Dai & Liu 2012)

    where t0is the starting time of the fall-back accretion in the central engine frame,M˙pis the peak of fall-back rate, and tpis the peak time of fall-back rate in the central engine frame.

    Progenitor envelope material falls back in the late time and forms an accretion disk,which will be viscous accretion by the BH.The accretion rate can be obtained as(Kumar et al.2008a)

    where τvis~1/αΩkis viscous timescale of accretion disk.α is a standard dimensionless viscosity parameter with values of~0.01–0.1, and Ωkis the Kepler angular velocity of the accretion disk.Due to accretion disk mass Mdwill increase with the fall-back from the envelope material and decrease with accretion.Therefore, (Kumar et al.2008a; Lei et al.2017)

    The fall-back accretion can continuously extract the rotational energy of the BH through the BZ mechanism, and powers a Poynting dominated jet.A part of jet energy would undergo the internal dissipation process, which may generate the observed giant X-ray bump.To connect the observed X-ray luminosity LXand BZ power PBZ, it is necessary to introduce efficiency factor ηXand jet beaming factor fb

    where a?is the dimensionless BH spin parameter,m?=M?/M⊙is the dimensionless BH mass, and B?,15is strength of the magnetic field near the BH horizon in units of 1015G.From the Equations(8)and(9),it can be seen that the BZ power mainly depends on parameters of B?, m?and a?.

    In general, the strength of the magnetic field near the BH horizon can be estimated by balancing the magnetic pressure on the BH horizon and ram pressure of the accretion flow at the inner edge of the accretion disk (Moderski et al.1997)

    Figure 2.The fitting result of GRB 220117A’s X-ray re-brightening segment by adopted the fall-back accretion model.

    The BZ process extracts rotational energy and angular momentum from the BH,while the accretion process brings the energy and angular momentum of the accretion disk into the BH.According to the conservation of energy and angular momentum, the evolution of BH under the two processes can be written as (Wang et al.2002)

    with

    4.Model Application to the X-Ray Re-brightening Signature of GRB 220117A

    In this section, we apply the fall-back accretion model that was introduced in Section 3 to the X-ray re-brightening segment and follow-up segment of GRB 220117A.We adopt the start time of re-brightening segment tstart=tstart,obs/(1+z) and the end time of follow-up segment tend=tend,obs/(1+z) as the start time and the end time of the fall-back accretion in the central engine frame.According to analysis, the initial mass of BH hardly affects the BZ power.In this section, we adopt M?,0=3M⊙.In addition, we take fb=0.01 and ηX=0.01 in our calculation.Finally, we take the dimensionless peak fallback ratem˙p, the sharpness of the peak s, the peak time of fallback rate tpand initial BH spin a0as our free parameters.In order to obtain the best fitting values, a Markov Chain Monte Carlo (MCMC) method is adopted.In our MCMC fitting, the emcee code is used (Foreman-Mackey et al.2013).In the code, we set the boundaries of four free parameters to log10(m˙p) ≡ [- 1 5, 0], s ≡[0, 10], tp≡[tstart, tend] and a0≡[0,1], respectively.

    Figure 3.The corner plot of the free parameters posterior probability distribution for the fitting result.

    The fallback accretion rate reaches a peak value~1.70×10-5M⊙s-1around 300 s in the central engine frame.The bounding shock responsible for the associated supernova transfers kinetic energy to the envelope materials and most of the envelope materials would be ejected.Therefore, it is very necessary to check whether the progenitor of GRB 220117A can provide enough envelope material.The fall-back rate of envelope material can be estimated by the data of pre-SN models, i.e., (Suwa & Ioka 2011; Woosley & Heger 2012;Matsumoto et al.2015; Liu et al.2018)

    where ρ is the density of envelope material at radius r.We set the time and radial coordinate for which the enclosed mass reach initial black hole mass as r0and 0,respectively.By adopt the progenitor density profile with different metallicities and masses from Liu et al.(2018), we calculate evolution of the mass supply rate for theirs and are shown in Figure 4.We find that low-metallicity massive progenitor stars are compatible with our fitting results.

    Figure 4.The evolution of the mass supply rate of progenitor with different metallicities and masses.The dashed line represents fall-back rate evolution of GRB 220117A’s progenitor envelope material in our fitting.Z⊙is the metallicities of the Sun.

    5.Discussion and Conclusions

    The Swift/XRT detected the X-ray afterglow of long burst GRB 220117A, which began to rebrighten 300 s after triggering and followed a single power-law decay segment after thousands of seconds of the orbital observation gap.The re-brightening segment is different from the shallow decay segment (plateau) and flare, and may belong to a giant X-ray bump.We investigated this segment by the fall-back accretion energy internal dissipation model.We found that the model can interpret this segment with reasonable parameter values.Within this physical model scenario,the fallback accretion rate reaches a peak value ~1.70×10-5M⊙s-1around 300 s in the central engine frame, which is compatible with the late mass supply rate of some low-metallicity massive progenitor stars.The initial BH spin isand implies that this rebrightening signature requires a larger BH spin.The total accretion mass Maccduring the fall-back process is Macc=3.09×10-2M⊙.The jet energy from the fall-back accretion is(9.77±0.65)×1052erg,with a ratio of 0.066 to the isotropic-equivalent radiation energies of GRB prompt phase in the 1–104keV band.The fall-back radius rpcorresponding to tpis (3.16±0.05)×1010cm, which is consistent with the typical radius of Wolf–Rayet stars.In summary, our results provide additional support for the origin of the long burst from the core collapse of Wolf–Rayet stars,and its late central engine activity is likely due to the fall-back accretion process.

    In this paper, we adopted a simple fall-back accretion rate evolution model, and do not consider the angular momentum distribution of the progenitor star, so this calculation is approximately valid for a slowly rotating progenitor.In fact,the angular velocities Ω of stars with different radii are different and the fall-back radius satisfies ∝Ω2(Kumar et al.2008a).Therefore,the angular momentum distribution of the progenitor star has a great influence on the fall-back accretion rate.In addition, the metallicities and masses of stars will have a certain impact on the fall-back accretion rate of the envelope material.In the future, we will study the fall-back accretion model with different angular momentum distribution, mass distribution and metallicity.

    Super Eddington accretion makes material on the accretion disk subject to an outward radiation pressure that is greater than gravity, Therefore, an outflow (i.e., disk wind) driven by radiation pressure is launched on the surface of the accretion disk, and taking away a part of the fall-back materials.However, the disk wind is ignored in the fall-back accretion model adopted in this paper.It will cause the accretion rate of BH to decrease.Because the outflow of the accretion disk is not well understood, the power law function model is generally adopted to describe the accretion rate at different accretion disk radii.It can be seen that the influence from the outflow of the accretion disk to the accretion rate is highly dependent on the power law index.In addition, the existence of the accretion disk outflow will also be important for understanding the baryon load of a GRB jet (Lei et al.2013, 2017) and56Ni synthesis for associated supernovae (Song & Liu 2019).We hope that the future general-relativistic magnetohydrodynamic(GRMHD) simulations can help us better understand the accretion disk outflow.

    免费看a级黄色片| 亚洲熟妇熟女久久| 亚洲 欧美 日韩 在线 免费| 老司机午夜福利在线观看视频| 国产亚洲精品久久久久5区| 国产在线观看jvid| 美女 人体艺术 gogo| 听说在线观看完整版免费高清| 国产av一区二区精品久久| 黑人巨大精品欧美一区二区mp4| 中文字幕av在线有码专区| 首页视频小说图片口味搜索| 男插女下体视频免费在线播放| 亚洲av熟女| 国产午夜精品久久久久久| 国产又色又爽无遮挡免费看| 国产午夜福利久久久久久| 女人爽到高潮嗷嗷叫在线视频| 99久久综合精品五月天人人| 女警被强在线播放| 亚洲国产欧美人成| 麻豆久久精品国产亚洲av| 在线观看舔阴道视频| 淫妇啪啪啪对白视频| 性欧美人与动物交配| 毛片女人毛片| 在线观看美女被高潮喷水网站 | 成人特级黄色片久久久久久久| 搡老熟女国产l中国老女人| 国产av一区在线观看免费| 美女 人体艺术 gogo| 1024视频免费在线观看| 久久香蕉国产精品| 国产主播在线观看一区二区| 国产午夜福利久久久久久| 中文字幕久久专区| 一夜夜www| 日韩三级视频一区二区三区| av国产免费在线观看| 夜夜看夜夜爽夜夜摸| 久久精品亚洲精品国产色婷小说| 亚洲成a人片在线一区二区| 久久久久久久精品吃奶| 女生性感内裤真人,穿戴方法视频| 欧美黑人欧美精品刺激| 免费电影在线观看免费观看| 国产在线观看jvid| 日韩成人在线观看一区二区三区| 成人国产一区最新在线观看| 欧美三级亚洲精品| 久热爱精品视频在线9| 手机成人av网站| 色老头精品视频在线观看| 日韩欧美精品v在线| 久久久久久人人人人人| 亚洲专区国产一区二区| 国产亚洲精品综合一区在线观看 | 欧美日韩一级在线毛片| 69av精品久久久久久| 欧美一区二区国产精品久久精品 | 午夜福利在线在线| av免费在线观看网站| 无限看片的www在线观看| 精品国产乱子伦一区二区三区| 国内久久婷婷六月综合欲色啪| 国产精品亚洲av一区麻豆| 中出人妻视频一区二区| 老司机午夜福利在线观看视频| 国产精品永久免费网站| 久久性视频一级片| 一个人观看的视频www高清免费观看 | 成人av一区二区三区在线看| 欧美高清成人免费视频www| 成人国语在线视频| 桃红色精品国产亚洲av| 一二三四社区在线视频社区8| 亚洲精品中文字幕在线视频| 亚洲avbb在线观看| 免费在线观看成人毛片| cao死你这个sao货| 国产成人精品久久二区二区91| 久久中文字幕一级| 淫秽高清视频在线观看| 麻豆国产97在线/欧美 | 国产精品一区二区三区四区免费观看 | 黄色成人免费大全| 欧美性长视频在线观看| 欧美绝顶高潮抽搐喷水| 男女那种视频在线观看| 亚洲精品国产一区二区精华液| 18禁黄网站禁片午夜丰满| 最近在线观看免费完整版| 听说在线观看完整版免费高清| 亚洲av美国av| 两个人免费观看高清视频| 亚洲欧美日韩无卡精品| 久久久久久九九精品二区国产 | 在线看三级毛片| 51午夜福利影视在线观看| 日韩欧美免费精品| 国产精品日韩av在线免费观看| 波多野结衣高清作品| 国产成年人精品一区二区| 国产免费av片在线观看野外av| 少妇粗大呻吟视频| 熟女电影av网| 婷婷精品国产亚洲av| 国产亚洲精品av在线| 亚洲国产欧美人成| 亚洲av日韩精品久久久久久密| 国产又色又爽无遮挡免费看| 亚洲精品在线观看二区| 午夜影院日韩av| 婷婷精品国产亚洲av在线| 国产三级在线视频| 精品人妻1区二区| 一边摸一边做爽爽视频免费| 婷婷亚洲欧美| 久久久久久久久中文| 老司机午夜十八禁免费视频| 亚洲一卡2卡3卡4卡5卡精品中文| 国产精品久久视频播放| 久久久久久久午夜电影| 99精品欧美一区二区三区四区| 国产黄片美女视频| 欧美精品啪啪一区二区三区| 在线观看免费视频日本深夜| 757午夜福利合集在线观看| 久久久久久免费高清国产稀缺| 精品国产乱子伦一区二区三区| 黄色a级毛片大全视频| 给我免费播放毛片高清在线观看| 午夜精品久久久久久毛片777| 一本久久中文字幕| 青草久久国产| 久久久久国内视频| 精品国产亚洲在线| 99热这里只有是精品50| 日本 欧美在线| 亚洲片人在线观看| 国产成+人综合+亚洲专区| 夜夜夜夜夜久久久久| 亚洲七黄色美女视频| 搡老岳熟女国产| 免费无遮挡裸体视频| 午夜免费激情av| 久久久水蜜桃国产精品网| 亚洲 国产 在线| xxxwww97欧美| 90打野战视频偷拍视频| 欧美一区二区精品小视频在线| 国语自产精品视频在线第100页| 亚洲电影在线观看av| 亚洲成人久久性| 男人舔奶头视频| 很黄的视频免费| 一进一出抽搐gif免费好疼| 深夜精品福利| 亚洲 国产 在线| 巨乳人妻的诱惑在线观看| 妹子高潮喷水视频| 在线观看www视频免费| 久久久久久久久免费视频了| 欧美一级a爱片免费观看看 | 五月玫瑰六月丁香| 中文字幕精品亚洲无线码一区| 国产精品久久久久久亚洲av鲁大| 男人舔奶头视频| 国产精品综合久久久久久久免费| 免费av毛片视频| 免费电影在线观看免费观看| 精华霜和精华液先用哪个| 19禁男女啪啪无遮挡网站| 麻豆国产97在线/欧美 | 90打野战视频偷拍视频| 精品久久久久久,| 国产av不卡久久| 男女床上黄色一级片免费看| 欧美日韩中文字幕国产精品一区二区三区| 久久久久久久精品吃奶| 中亚洲国语对白在线视频| 欧美日韩一级在线毛片| 18禁黄网站禁片午夜丰满| 久9热在线精品视频| 欧洲精品卡2卡3卡4卡5卡区| 黄色丝袜av网址大全| 黄片大片在线免费观看| 日韩三级视频一区二区三区| 舔av片在线| 最近在线观看免费完整版| 亚洲人与动物交配视频| 久久香蕉激情| 精品欧美一区二区三区在线| 久久久精品国产亚洲av高清涩受| 欧美乱妇无乱码| 亚洲人与动物交配视频| 97超级碰碰碰精品色视频在线观看| 久久午夜综合久久蜜桃| 久久久久久久久免费视频了| 日韩欧美国产在线观看| 国产午夜福利久久久久久| 国产精品1区2区在线观看.| 亚洲国产精品合色在线| 91老司机精品| 欧美一级毛片孕妇| 最新在线观看一区二区三区| 国产精品一区二区免费欧美| 脱女人内裤的视频| svipshipincom国产片| 伦理电影免费视频| 无限看片的www在线观看| 欧美乱色亚洲激情| 色老头精品视频在线观看| 亚洲最大成人中文| 黑人操中国人逼视频| 亚洲一卡2卡3卡4卡5卡精品中文| 男人的好看免费观看在线视频 | 精品国产乱子伦一区二区三区| 高清在线国产一区| 亚洲免费av在线视频| 法律面前人人平等表现在哪些方面| 中文字幕最新亚洲高清| 久久国产精品人妻蜜桃| 国产伦一二天堂av在线观看| 国产精品1区2区在线观看.| 亚洲美女黄片视频| 人人妻人人澡欧美一区二区| 精品国产美女av久久久久小说| 天堂√8在线中文| av在线天堂中文字幕| 久久精品国产亚洲av高清一级| 毛片女人毛片| 欧美色视频一区免费| 欧美大码av| 可以在线观看毛片的网站| 婷婷亚洲欧美| 欧美在线黄色| 国产精品香港三级国产av潘金莲| 女生性感内裤真人,穿戴方法视频| 香蕉丝袜av| 99精品欧美一区二区三区四区| 久久亚洲真实| 人成视频在线观看免费观看| 国产精品久久久久久人妻精品电影| 男女之事视频高清在线观看| 久久香蕉激情| 50天的宝宝边吃奶边哭怎么回事| 亚洲一区二区三区不卡视频| 天天躁夜夜躁狠狠躁躁| 97人妻精品一区二区三区麻豆| 久久精品aⅴ一区二区三区四区| 亚洲七黄色美女视频| 久久精品91无色码中文字幕| 狂野欧美激情性xxxx| 波多野结衣巨乳人妻| 91字幕亚洲| 男人舔女人下体高潮全视频| 深夜精品福利| cao死你这个sao货| 久久久国产成人免费| 国产成人av激情在线播放| 丁香六月欧美| 色尼玛亚洲综合影院| 91在线观看av| 国产午夜福利久久久久久| 久久99热这里只有精品18| 久久精品综合一区二区三区| 男女之事视频高清在线观看| 最新在线观看一区二区三区| 观看免费一级毛片| 手机成人av网站| www.自偷自拍.com| 国产主播在线观看一区二区| 老汉色av国产亚洲站长工具| 亚洲一码二码三码区别大吗| 狂野欧美激情性xxxx| 免费在线观看视频国产中文字幕亚洲| 女人高潮潮喷娇喘18禁视频| 99热只有精品国产| 免费看十八禁软件| 国产黄色小视频在线观看| 男插女下体视频免费在线播放| 可以免费在线观看a视频的电影网站| 日韩欧美在线二视频| 淫妇啪啪啪对白视频| 久热爱精品视频在线9| 一区二区三区高清视频在线| 一进一出好大好爽视频| 国产av不卡久久| 日本免费a在线| 亚洲国产欧洲综合997久久,| 天天添夜夜摸| 母亲3免费完整高清在线观看| 在线看三级毛片| 国产久久久一区二区三区| 韩国av一区二区三区四区| 三级男女做爰猛烈吃奶摸视频| 在线观看免费视频日本深夜| 美女午夜性视频免费| 中文字幕熟女人妻在线| 欧美色欧美亚洲另类二区| 日本一本二区三区精品| 老司机深夜福利视频在线观看| 国产成+人综合+亚洲专区| 99久久久亚洲精品蜜臀av| 国产91精品成人一区二区三区| 国产一区二区三区在线臀色熟女| 久99久视频精品免费| 午夜精品在线福利| 成年免费大片在线观看| 成人欧美大片| 欧美不卡视频在线免费观看 | 国产亚洲精品久久久久久毛片| 日本黄色视频三级网站网址| 神马国产精品三级电影在线观看 | 久久久久久亚洲精品国产蜜桃av| 啦啦啦韩国在线观看视频| 国产午夜福利久久久久久| 在线永久观看黄色视频| 一夜夜www| 国产成人aa在线观看| 首页视频小说图片口味搜索| 一级毛片女人18水好多| 777久久人妻少妇嫩草av网站| 亚洲自拍偷在线| 欧美日韩中文字幕国产精品一区二区三区| 亚洲成人国产一区在线观看| a级毛片在线看网站| 久久这里只有精品19| 亚洲av成人精品一区久久| 在线十欧美十亚洲十日本专区| 国产三级中文精品| 亚洲成人中文字幕在线播放| 国产精品自产拍在线观看55亚洲| 久99久视频精品免费| 午夜精品久久久久久毛片777| 国内精品久久久久久久电影| 女人被狂操c到高潮| 久久伊人香网站| av福利片在线观看| 国产精品香港三级国产av潘金莲| 男女视频在线观看网站免费 | 后天国语完整版免费观看| 色尼玛亚洲综合影院| 国产亚洲av高清不卡| avwww免费| 露出奶头的视频| a级毛片在线看网站| 狂野欧美激情性xxxx| 精品一区二区三区av网在线观看| 国产精品亚洲一级av第二区| 亚洲专区中文字幕在线| 两个人免费观看高清视频| 大型av网站在线播放| 成人国语在线视频| netflix在线观看网站| 国产一级毛片七仙女欲春2| 久久精品aⅴ一区二区三区四区| 99精品欧美一区二区三区四区| 嫁个100分男人电影在线观看| 熟女少妇亚洲综合色aaa.| 亚洲国产中文字幕在线视频| 精品高清国产在线一区| 我的老师免费观看完整版| 欧美黑人精品巨大| 嫩草影院精品99| 国产亚洲av嫩草精品影院| 久久国产精品人妻蜜桃| 亚洲熟女毛片儿| 亚洲片人在线观看| 人成视频在线观看免费观看| 欧美日韩亚洲国产一区二区在线观看| 欧美成人免费av一区二区三区| 国产精品野战在线观看| 久久国产精品人妻蜜桃| 久久精品人妻少妇| 舔av片在线| 97超级碰碰碰精品色视频在线观看| 精品国内亚洲2022精品成人| 亚洲精品在线观看二区| 亚洲精品美女久久久久99蜜臀| 色精品久久人妻99蜜桃| 怎么达到女性高潮| 国产精品久久久久久久电影 | 五月伊人婷婷丁香| 天天添夜夜摸| 女人被狂操c到高潮| 一区二区三区激情视频| 久久久久久九九精品二区国产 | 亚洲国产精品成人综合色| 91麻豆av在线| 两性午夜刺激爽爽歪歪视频在线观看 | 一个人观看的视频www高清免费观看 | 午夜激情av网站| 丰满的人妻完整版| 99国产综合亚洲精品| 成年女人毛片免费观看观看9| 激情在线观看视频在线高清| 天堂动漫精品| 97超级碰碰碰精品色视频在线观看| 婷婷亚洲欧美| 国产不卡一卡二| 欧美日韩乱码在线| 夜夜夜夜夜久久久久| 观看免费一级毛片| 每晚都被弄得嗷嗷叫到高潮| 一二三四社区在线视频社区8| 欧美成人一区二区免费高清观看 | 夜夜躁狠狠躁天天躁| 国产视频一区二区在线看| 亚洲激情在线av| 午夜免费激情av| 校园春色视频在线观看| 一本综合久久免费| 搡老岳熟女国产| 黄频高清免费视频| 日本三级黄在线观看| 成人特级黄色片久久久久久久| 一个人免费在线观看的高清视频| 亚洲欧美日韩东京热| 亚洲,欧美精品.| 成人手机av| 九色国产91popny在线| 欧美成人午夜精品| 国产成年人精品一区二区| 在线永久观看黄色视频| 精品欧美国产一区二区三| 国产精品自产拍在线观看55亚洲| 亚洲国产精品久久男人天堂| 欧美三级亚洲精品| 国产一区二区三区视频了| 免费看美女性在线毛片视频| 亚洲欧美激情综合另类| 精品久久久久久久人妻蜜臀av| 久久久久亚洲av毛片大全| 亚洲狠狠婷婷综合久久图片| 在线观看日韩欧美| 波多野结衣巨乳人妻| av国产免费在线观看| 国产精品 国内视频| 日日夜夜操网爽| 97人妻精品一区二区三区麻豆| 香蕉国产在线看| 亚洲精品av麻豆狂野| 999久久久国产精品视频| 久久久水蜜桃国产精品网| 精品一区二区三区四区五区乱码| 亚洲国产日韩欧美精品在线观看 | 亚洲人成网站在线播放欧美日韩| 免费在线观看完整版高清| 婷婷丁香在线五月| 久久精品国产综合久久久| 他把我摸到了高潮在线观看| 午夜免费激情av| 国内精品一区二区在线观看| 免费在线观看完整版高清| 久久久久国产一级毛片高清牌| 亚洲国产精品sss在线观看| 国产黄色小视频在线观看| www.熟女人妻精品国产| 成人特级黄色片久久久久久久| 国产成年人精品一区二区| 一二三四在线观看免费中文在| 精品乱码久久久久久99久播| 亚洲精品久久国产高清桃花| 国产av一区在线观看免费| 婷婷亚洲欧美| 亚洲精品美女久久久久99蜜臀| 无人区码免费观看不卡| 黄色a级毛片大全视频| 男人舔奶头视频| 美女黄网站色视频| 好男人在线观看高清免费视频| 亚洲一区二区三区不卡视频| 少妇人妻一区二区三区视频| 大型av网站在线播放| 日韩欧美在线乱码| 色在线成人网| 国产精品久久久久久人妻精品电影| 黄色a级毛片大全视频| 神马国产精品三级电影在线观看 | 91av网站免费观看| 久久久久性生活片| 亚洲一区二区三区不卡视频| 婷婷六月久久综合丁香| 久久精品综合一区二区三区| 中出人妻视频一区二区| 亚洲午夜理论影院| 黄色女人牲交| 精品乱码久久久久久99久播| 成熟少妇高潮喷水视频| 亚洲av五月六月丁香网| av在线天堂中文字幕| 精品一区二区三区av网在线观看| 国产成人av激情在线播放| 婷婷精品国产亚洲av在线| 制服丝袜大香蕉在线| 日本在线视频免费播放| 每晚都被弄得嗷嗷叫到高潮| 国产黄色小视频在线观看| 50天的宝宝边吃奶边哭怎么回事| 三级男女做爰猛烈吃奶摸视频| 十八禁网站免费在线| 男女视频在线观看网站免费 | 精品国产亚洲在线| 欧美av亚洲av综合av国产av| 国产精品久久视频播放| 黄色丝袜av网址大全| 久久久久久九九精品二区国产 | 欧美性猛交黑人性爽| tocl精华| 欧美乱色亚洲激情| 久久99热这里只有精品18| av国产免费在线观看| 在线观看免费日韩欧美大片| 国产精品一区二区免费欧美| 成人国产一区最新在线观看| 欧美日韩乱码在线| 亚洲国产精品成人综合色| 一区二区三区国产精品乱码| 亚洲美女黄片视频| 天天添夜夜摸| xxx96com| 日韩欧美 国产精品| 男女之事视频高清在线观看| 久久草成人影院| 婷婷亚洲欧美| 午夜影院日韩av| 男人的好看免费观看在线视频 | 国产片内射在线| 欧美一级a爱片免费观看看 | 中文字幕av在线有码专区| 成人精品一区二区免费| 亚洲国产精品999在线| 香蕉av资源在线| 最近最新免费中文字幕在线| 成人18禁在线播放| 国产成+人综合+亚洲专区| 一进一出好大好爽视频| 成人手机av| 黄色毛片三级朝国网站| 国产蜜桃级精品一区二区三区| 嫁个100分男人电影在线观看| 在线观看舔阴道视频| 我的老师免费观看完整版| a级毛片在线看网站| 欧美极品一区二区三区四区| 搞女人的毛片| 午夜a级毛片| 国产97色在线日韩免费| 小说图片视频综合网站| 99热只有精品国产| 成人午夜高清在线视频| 欧美色欧美亚洲另类二区| 妹子高潮喷水视频| www.自偷自拍.com| 国产精品精品国产色婷婷| 人妻丰满熟妇av一区二区三区| 国产精品久久久久久亚洲av鲁大| 91av网站免费观看| 欧洲精品卡2卡3卡4卡5卡区| 午夜影院日韩av| 一个人免费在线观看的高清视频| 色尼玛亚洲综合影院| 一级a爱片免费观看的视频| 少妇的丰满在线观看| 又紧又爽又黄一区二区| 久久婷婷人人爽人人干人人爱| 久久久久性生活片| 国产一级毛片七仙女欲春2| 天堂√8在线中文| www.熟女人妻精品国产| 国产一级毛片七仙女欲春2| 床上黄色一级片| 狂野欧美白嫩少妇大欣赏| 欧美乱码精品一区二区三区| 亚洲精品美女久久久久99蜜臀| 欧美丝袜亚洲另类 | 亚洲中文av在线| 日韩欧美在线二视频| 国产视频一区二区在线看| 国产蜜桃级精品一区二区三区| 成年人黄色毛片网站| 午夜成年电影在线免费观看| 国产免费男女视频| 一区二区三区激情视频| 亚洲av成人av| 亚洲精品国产一区二区精华液| 婷婷精品国产亚洲av在线| 麻豆国产av国片精品| 国语自产精品视频在线第100页| 亚洲国产欧美人成| 最近最新中文字幕大全电影3| 亚洲片人在线观看| 午夜精品久久久久久毛片777| 两性午夜刺激爽爽歪歪视频在线观看 | 成年女人毛片免费观看观看9| 妹子高潮喷水视频| 色播亚洲综合网| svipshipincom国产片| 国产精品1区2区在线观看.| 免费高清视频大片| 成人国语在线视频| 久久午夜亚洲精品久久| 99精品久久久久人妻精品| 久久久久精品国产欧美久久久| 欧美3d第一页| 久久精品国产99精品国产亚洲性色| 一进一出抽搐动态| 免费在线观看日本一区| 一卡2卡三卡四卡精品乱码亚洲| 中文字幕av在线有码专区| 999精品在线视频| av超薄肉色丝袜交足视频| 丁香六月欧美|