adsabs/AstroCLIMB huggingface dataset:
Paper: On the Robustness of the Velocity Anisotropy Parameter in Probing the Stellar Kinematics in Milky Way–Like Galaxies: Takeaway from TNG50 Simulation
Authors: Razieh Emami, Lars Hernquist, Mark Vogelsberger, Xuejian Shen, Joshua S. Speagle, 佳士 沈, Jorge Moreno, Charles Alcock, Shy Genel, John C. Forbes, Federico Marinacci, Paul Torrey
Figure caption: The β radial profile for stars inferred using different selection criteria. Dashed black, blue dotted–dashed, solid red, and dotted yellow lines present β inferred from stars with kinematic, metallicity-based, spatial cut, and no cut as was used in computing the β, respectively.
Paper: On the Robustness of the Velocity Anisotropy Parameter in Probing the Stellar Kinematics in Milky Way–Like Galaxies: Takeaway from TNG50 Simulation
Authors: Razieh Emami, Lars Hernquist, Mark Vogelsberger, Xuejian Shen, Joshua S. Speagle, 佳士 沈, Jorge Moreno, Charles Alcock, Shy Genel, John C. Forbes, Federico Marinacci, Paul Torrey
Figure caption: (Left panel) Profile of β with a monotonically increasing radial profile; 32% of the halos are in this category. Almost all of them are from category ﹩{ \mathcal A }﹩, with one exception belonging to class ﹩{ \mathcal B }﹩. (Right panel) β radial profile for cases with peaks and troughs. About 68% of the halos belong to this category, of which only 29% belong to category ﹩{ \mathcal A }﹩. This means that care must be taken in interpreting the observed peaks/troughs in the β radial profile, as it might be an indication of different selection criteria.
Paper: On the Robustness of the Velocity Anisotropy Parameter in Probing the Stellar Kinematics in Milky Way–Like Galaxies: Takeaway from TNG50 Simulation
Authors: Razieh Emami, Lars Hernquist, Mark Vogelsberger, Xuejian Shen, Joshua S. Speagle, 佳士 沈, Jorge Moreno, Charles Alcock, Shy Genel, John C. Forbes, Federico Marinacci, Paul Torrey
Figure caption: Radial profile of ﹩{\rm{\Delta }}\beta (r)\equiv \left({\beta }^{\mathrm{Fe}}/{\beta }^{\mathrm{No}-\mathrm{cut}}\right)(r)-1﹩ for halos from different categories. As stated in Section 4.1.1, halos from categories ﹩{ \mathcal A }﹩–﹩{ \mathcal C }﹩ show little to very strong response on different selection criteria for β. In addition, it is inferred that, on average, halos from category ﹩{ \mathcal A }﹩ show smoother radial profiles than the other two classes. This is clarified in Figure 8.
Paper: On the Robustness of the Velocity Anisotropy Parameter in Probing the Stellar Kinematics in Milky Way–Like Galaxies: Takeaway from TNG50 Simulation
Authors: Razieh Emami, Lars Hernquist, Mark Vogelsberger, Xuejian Shen, Joshua S. Speagle, 佳士 沈, Jorge Moreno, Charles Alcock, Shy Genel, John C. Forbes, Federico Marinacci, Paul Torrey
Figure caption: The 2D correlation of the stellar distance vs. stellar metallicity for a subsample of four galaxies from our MW-like galaxy sample. The Spearman correlation is modest and negative, indicating that metal-rich stars are located closer to the galactic center.
Paper: On the Robustness of the Velocity Anisotropy Parameter in Probing the Stellar Kinematics in Milky Way–Like Galaxies: Takeaway from TNG50 Simulation
Authors: Razieh Emami, Lars Hernquist, Mark Vogelsberger, Xuejian Shen, Joshua S. Speagle, 佳士 沈, Jorge Moreno, Charles Alcock, Shy Genel, John C. Forbes, Federico Marinacci, Paul Torrey
Figure caption: Face-on (left) and (two) edge-on (middle-right) projections of stars in galaxy 1 in our sample. Down rows present the spatial distribution of stars from ﹩\tilde{r}\geqslant 1﹩, ﹩\tilde{r}\geqslant 1,\epsilon \leqslant 0.7﹩, ﹩\tilde{r}\geqslant 1,\tilde{Z}\geqslant 5﹩ and ﹩\tilde{r}\geqslant 1,\tilde{Z}\geqslant 5,﹩ [Fe/H] ≤ −1.3. The color bars refer to the surface number density of stars in different projections.
Paper: On the Robustness of the Velocity Anisotropy Parameter in Probing the Stellar Kinematics in Milky Way–Like Galaxies: Takeaway from TNG50 Simulation
Authors: Razieh Emami, Lars Hernquist, Mark Vogelsberger, Xuejian Shen, Joshua S. Speagle, 佳士 沈, Jorge Moreno, Charles Alcock, Shy Genel, John C. Forbes, Federico Marinacci, Paul Torrey
Figure caption: The 2D correlation of the stellar velocity amplitude vs. the stellar metallicity for a subsample of four galaxies from our MW-like galaxy sample. It is inferred that the stellar velocity is largely uncorrelated with the stellar metallicity, as stellar speed is mainly concentrated between 200 and 300 km s−1, in agreement with the observed rotational velocity of stars in our MW.
Paper: On the Robustness of the Velocity Anisotropy Parameter in Probing the Stellar Kinematics in Milky Way–Like Galaxies: Takeaway from TNG50 Simulation
Authors: Razieh Emami, Lars Hernquist, Mark Vogelsberger, Xuejian Shen, Joshua S. Speagle, 佳士 沈, Jorge Moreno, Charles Alcock, Shy Genel, John C. Forbes, Federico Marinacci, Paul Torrey
Figure caption: Probability density distribution of stellar metallicity in our MW-like galaxy sample. It is evident that stars from different galaxies have quite similar metallicity distributions. Different colors refer to various galaxies. Low metallicities are in the tail of the distribution.
Paper: On the Robustness of the Velocity Anisotropy Parameter in Probing the Stellar Kinematics in Milky Way–Like Galaxies: Takeaway from TNG50 Simulation
Authors: Razieh Emami, Lars Hernquist, Mark Vogelsberger, Xuejian Shen, Joshua S. Speagle, 佳士 沈, Jorge Moreno, Charles Alcock, Shy Genel, John C. Forbes, Federico Marinacci, Paul Torrey
Figure caption: The 2D correlation of stellar age vs. metallicity for a subsample of four galaxies from our MW-like galaxy sample. The Spearman correlation is negative, indicating that metal-poor stars are older than metal-rich ones.
Paper: CLEAR: The Evolution of Spatially Resolved Star Formation in Galaxies between 0.5 ≲ z ≲ 1.7 Using Hα Emission Line Maps
Authors: Jasleen Matharu, Casey Papovich, Raymond C. Simons, Ivelina Momcheva, Gabriel Brammer, Zhiyuan Ji, Bren E. Backhaus, Nikko J. Cleri, Vicente Estrada-Carpenter, Steven L. Finkelstein, Kristian Finlator, Mauro Giavalisco, Intae Jung, Adam Muzzin, Erica J. Nelson, Annalisa Pillepich, Jonathan R. Trump, Benjamin Weiner
Figure caption: Left: the stellar mass–size (top row) and Σ1kpc–stellar mass relations (third row) for the stellar continuum and Hα emission measured at z ∼ 0.5 from CLEAR and at z ∼ 1 from 3D-HST. Dotted lines delineate 68% confidence intervals on the best-fit lines. Purple and orange shaded regions show z = 0.5 and z = 1 TNG50 measurements from Pillepich et al. (2019) applied to a galaxy sample matched to the observed ones. The second and fourth rows show log(R  eff,CLEAR )-log(R  eff,3D−HST) and log(Σ1kpc,3D−HST)-log(Σ1kpc,CLEAR), respectively, with the solid line showing the stellar mass range over which there are measurements from both surveys/comparable samples from TNG50. The numbers are the gradients of the lines. Both in the observations and simulations, the majority of the evolution with redshift is in Hα, with two-times larger difference between z ∼ 0.5 and z ∼ 1 in observed log(R eff) and 1.4-times larger difference between z ∼ 0.5 and z ∼ 1 in TNG50 log(R eff). The significance of the redshift evolution in Hα at a fixed stellar mass of log(M */M ⊙) = 9.5 is 2σ in the observations and 1σ−2σ in TNG50. For log(Σ1kpc), there is also a two-times larger difference in Hα between z ∼ 0.5 and z ∼ 1 than the stellar continuum. See Table 4 for the measured relations shown as solid lines in the first and third rows. Upper right: the ratio of the Hα-to-stellar continuum effective radius in CLEAR, 3D-HST, and TNG50. The IllustrisTNG effective radii follow the observational effective radii measurements remarkably well, suggesting the observed redshift evolution toward more extended Hα profiles of star-forming galaxies at lower redshifts is not dust-driven (see Section 7.3.1).
Paper: Possibilities and Limitations of Kinematically Identifying Stars from Accreted Ultra-faint Dwarf Galaxies
Authors: Kaley Brauer, Hillary Diane Andales, Alexander P. Ji, Anna Frebel, Mohammad K. Mardini, Facundo A. Gómez, Brian W. O'Shea
Figure caption: Strength of association between different kinematic observables and the true cluster labels. Higher ω 2 values indicate a stronger association. L tot has consistently high ω 2 values, implying it is an important variable when seeking to find clustered stars that accreted together. ρ, ϕ, z and v  r , v  ϕ , v  z  are the radius and velocity in cylindrical coordinates, respectively. The importance of r and v is due to their correlation with total energy.
Paper: Possibilities and Limitations of Kinematically Identifying Stars from Accreted Ultra-faint Dwarf Galaxies
Authors: Kaley Brauer, Hillary Diane Andales, Alexander P. Ji, Anna Frebel, Mohammad K. Mardini, Facundo A. Gómez, Brian W. O'Shea
Figure caption: Strength of association between actions (J  r , J  z , J  ϕ , E) and the true cluster labels. Higher ω 2 values indicate a stronger association. E has the highest ω 2 values, implying it is the most important variable when seeking to find clustered stars that accreted together. Note that J  ϕ  is defined in axisymmetric potentials to be equivalent to L  z .
Paper: CLEAR: The Evolution of Spatially Resolved Star Formation in Galaxies between 0.5 ≲ z ≲ 1.7 Using Hα Emission Line Maps
Authors: Jasleen Matharu, Casey Papovich, Raymond C. Simons, Ivelina Momcheva, Gabriel Brammer, Zhiyuan Ji, Bren E. Backhaus, Nikko J. Cleri, Vicente Estrada-Carpenter, Steven L. Finkelstein, Kristian Finlator, Mauro Giavalisco, Intae Jung, Adam Muzzin, Erica J. Nelson, Annalisa Pillepich, Jonathan R. Trump, Benjamin Weiner
Figure caption: Schematic representation for the natural consequences of inside-out growth via star formation in star-forming galaxies that can explain the redshift evolution seen in our study at 0.5 < z < 1 (see Section 7.3.2 for more details). The inside-out cessation of star formation (orange) will follow behind the inside-out growth (blue), becoming significant at lower redshifts. Σ1kpc,Hα  will be more sensitive to the effects of inside-out quenching on the ionized gas (that is traced by Hα).
Paper: Possibilities and Limitations of Kinematically Identifying Stars from Accreted Ultra-faint Dwarf Galaxies
Authors: Kaley Brauer, Hillary Diane Andales, Alexander P. Ji, Anna Frebel, Mohammad K. Mardini, Facundo A. Gómez, Brian W. O'Shea
Figure caption: Left: z = 0 dynamics (energy and z-angular momentum) of all accreted star particles within 50 kpc of the Sun in simulation Cat-14, one of the 32 simulated Milky Way-mass galaxies. The color of each particle corresponds to the mass of the galaxy in which it formed. Star particles from the smallest galaxies, the UFDs, are seen in red. Right: J  r  and J  z  orbital actions for the same star particles.
Paper: Possibilities and Limitations of Kinematically Identifying Stars from Accreted Ultra-faint Dwarf Galaxies
Authors: Kaley Brauer, Hillary Diane Andales, Alexander P. Ji, Anna Frebel, Mohammad K. Mardini, Facundo A. Gómez, Brian W. O'Shea
Figure caption: Example of clustering results for one simulation (Cat-14) from one data set (accreted star particles from UFDs within 50 kpc of the Sun). Far left: star particles from true UFD remnants in dynamic phase space. Many of the particles are phase-mixed. Right: results from each of the seven clustering algorithms tested in this paper. Most of the clusters found by these algorithms, especially those at lower energy, do not correspond to true UFD remnants.
Paper: Possibilities and Limitations of Kinematically Identifying Stars from Accreted Ultra-faint Dwarf Galaxies
Authors: Kaley Brauer, Hillary Diane Andales, Alexander P. Ji, Anna Frebel, Mohammad K. Mardini, Facundo A. Gómez, Brian W. O'Shea
Figure caption:  z = 0 dynamics of star particles that originated from UFDs in one of our simulations (with a 50 kpc radial cut; see Section 2.4). The color of each particle corresponds to how long ago it was accreted by the Milky Way-mass host galaxy. Stars that were accreted more recently are, generally, of higher energy and less phase-mixed. Over time, the stars mix more in the phase space and are less identifiable by clustering algorithms.
Paper: Possibilities and Limitations of Kinematically Identifying Stars from Accreted Ultra-faint Dwarf Galaxies
Authors: Kaley Brauer, Hillary Diane Andales, Alexander P. Ji, Anna Frebel, Mohammad K. Mardini, Facundo A. Gómez, Brian W. O'Shea
Figure caption: Across all 32 simulations, ∼91% of the galaxies accreted by Milky Way-mass galaxies are ultra-faint dwarf galaxies. These small galaxies only contribute ∼7% of the accreted star particles, however. These fractions are roughly constant with radial cut.
Paper: An Insight-HXMT View of the mHz Quasi-regular Modulation Phenomenon in the Black Hole X-Ray Binary 4U 1630–47
Authors: Zi-xu Yang, Liang Zhang, Yue Huang, Qingcui Bu, Zhen Zhang, He-Xin Liu, Wei Yu, Peng-Ju Wang, Q. C. Zhao, L. Tao, Jin-Lu Qu, Shu Zhang, Shuang-Nan Zhang, Liming Song, Fangjun Lu, Xuelei Cao, Li Chen, Ce Cai, Zhi Chang, Tianxiang Chen, Yong Chen, Yupeng Chen, Yibao Chen, Weiwei Cui, Guoqiang Ding, Yuanyuan Du, Guanhua Gao, He Gao, Mingyu Ge, Yudong Gu, Ju Guan, Chengcheng Guo, Dawei Han, Jia Huo, Shumei Jia, Weichun Jiang, Jing Jin, Lingda Kong, Bing Li, Gang Li, Wei Li, Xian Li, Xufang Li, Zhengwei Li, Chengkui Li, Lin Lin, Congzhan Liu, Tipei Li, Xiaobo Li, Xiaohua Liang, Jinyuan Liao, Hongwei Liu, Xiaojing Liu, Xuefeng Lu, Qi Luo, Tao Luo, Binyuan Ma, RuiCan Ma, Xiang Ma, Bin Meng, Yi Nang, Jianyin Nie, Ge Ou, Xiaoqin Ren, Na Sai, Xinying Song, Liang Sun, Ying Tan, Youli Tuo, Chen Wang, Wenshuai Wang, Lingjun Wang, Yusa Wang, Jieshuang Wang, Xiangyang Wen, Bobing Wu, Baiyang Wu, Mei Wu, Shuo Xiao, Yupeng Xu, Shaolin Xiong, Sheng Yang, Yanji Yang, Qibin Yi, Qianqing Yin, Yuan You, Bing Zhang, Fan Zhang, Hongmei Zhang, Juan Zhang, Wanchang Zhang, Wei Zhang, Binbin Zhang, Peng Zhang, Yifei Zhang, Yuanhang Zhang, Haisheng Zhao, Xiaofan Zhao, Shijie Zheng, Dengke Zhou
Figure caption: Fractional rms (left) and characteristic frequency (right) of the mHz QRM as a function of photon energy. The green, blue, and red points represent the LE, ME, and HE data, respectively. The dotted line represents the best-fitted line with a function of ﹩f\,=\,A\ast \mathrm{log}(E)+B﹩. The fractional rms and characteristic frequency are measured from the PDS averaged from all the observations with the mHz QRM (ObsIDs P040426300901, P040426300902, P040426300903, P040426301001, P040426301002, P040426301003).
Paper: An Insight-HXMT View of the mHz Quasi-regular Modulation Phenomenon in the Black Hole X-Ray Binary 4U 1630–47
Authors: Zi-xu Yang, Liang Zhang, Yue Huang, Qingcui Bu, Zhen Zhang, He-Xin Liu, Wei Yu, Peng-Ju Wang, Q. C. Zhao, L. Tao, Jin-Lu Qu, Shu Zhang, Shuang-Nan Zhang, Liming Song, Fangjun Lu, Xuelei Cao, Li Chen, Ce Cai, Zhi Chang, Tianxiang Chen, Yong Chen, Yupeng Chen, Yibao Chen, Weiwei Cui, Guoqiang Ding, Yuanyuan Du, Guanhua Gao, He Gao, Mingyu Ge, Yudong Gu, Ju Guan, Chengcheng Guo, Dawei Han, Jia Huo, Shumei Jia, Weichun Jiang, Jing Jin, Lingda Kong, Bing Li, Gang Li, Wei Li, Xian Li, Xufang Li, Zhengwei Li, Chengkui Li, Lin Lin, Congzhan Liu, Tipei Li, Xiaobo Li, Xiaohua Liang, Jinyuan Liao, Hongwei Liu, Xiaojing Liu, Xuefeng Lu, Qi Luo, Tao Luo, Binyuan Ma, RuiCan Ma, Xiang Ma, Bin Meng, Yi Nang, Jianyin Nie, Ge Ou, Xiaoqin Ren, Na Sai, Xinying Song, Liang Sun, Ying Tan, Youli Tuo, Chen Wang, Wenshuai Wang, Lingjun Wang, Yusa Wang, Jieshuang Wang, Xiangyang Wen, Bobing Wu, Baiyang Wu, Mei Wu, Shuo Xiao, Yupeng Xu, Shaolin Xiong, Sheng Yang, Yanji Yang, Qibin Yi, Qianqing Yin, Yuan You, Bing Zhang, Fan Zhang, Hongmei Zhang, Juan Zhang, Wanchang Zhang, Wei Zhang, Binbin Zhang, Peng Zhang, Yifei Zhang, Yuanhang Zhang, Haisheng Zhao, Xiaofan Zhao, Shijie Zheng, Dengke Zhou
Figure caption: ME 8–35 keV light curve and the corresponding dynamical PDS for a particular period that shows fast transitions among different kinds of PDS. The bin size of the light curve is 80 s. In the top panel, the dashed lines mark the time gaps between orbits. In the bottom panel, the x-axis represents the index of each PDS. We divide this period into five epochs: epoch 1 (P040426300801), the period with a type C QPO in the PDS; epoch 2 (P040426300901, P040426301001, P040426301002), the period that shows a mHz QRM; epoch 3 (the first part of P040426301003), the period when mHz QRM disappears and the PDS is dominated by Poisson noise; epoch 4 (the last part of P040426301003), the period when the mHz QRM reappears, and epoch 5 (ObsID P040426301004), where QRM disappears again.
Paper: An Insight-HXMT View of the mHz Quasi-regular Modulation Phenomenon in the Black Hole X-Ray Binary 4U 1630–47
Authors: Zi-xu Yang, Liang Zhang, Yue Huang, Qingcui Bu, Zhen Zhang, He-Xin Liu, Wei Yu, Peng-Ju Wang, Q. C. Zhao, L. Tao, Jin-Lu Qu, Shu Zhang, Shuang-Nan Zhang, Liming Song, Fangjun Lu, Xuelei Cao, Li Chen, Ce Cai, Zhi Chang, Tianxiang Chen, Yong Chen, Yupeng Chen, Yibao Chen, Weiwei Cui, Guoqiang Ding, Yuanyuan Du, Guanhua Gao, He Gao, Mingyu Ge, Yudong Gu, Ju Guan, Chengcheng Guo, Dawei Han, Jia Huo, Shumei Jia, Weichun Jiang, Jing Jin, Lingda Kong, Bing Li, Gang Li, Wei Li, Xian Li, Xufang Li, Zhengwei Li, Chengkui Li, Lin Lin, Congzhan Liu, Tipei Li, Xiaobo Li, Xiaohua Liang, Jinyuan Liao, Hongwei Liu, Xiaojing Liu, Xuefeng Lu, Qi Luo, Tao Luo, Binyuan Ma, RuiCan Ma, Xiang Ma, Bin Meng, Yi Nang, Jianyin Nie, Ge Ou, Xiaoqin Ren, Na Sai, Xinying Song, Liang Sun, Ying Tan, Youli Tuo, Chen Wang, Wenshuai Wang, Lingjun Wang, Yusa Wang, Jieshuang Wang, Xiangyang Wen, Bobing Wu, Baiyang Wu, Mei Wu, Shuo Xiao, Yupeng Xu, Shaolin Xiong, Sheng Yang, Yanji Yang, Qibin Yi, Qianqing Yin, Yuan You, Bing Zhang, Fan Zhang, Hongmei Zhang, Juan Zhang, Wanchang Zhang, Wei Zhang, Binbin Zhang, Peng Zhang, Yifei Zhang, Yuanhang Zhang, Haisheng Zhao, Xiaofan Zhao, Shijie Zheng, Dengke Zhou
Figure caption: Frequency-dependent phase-lag spectra in different energy bands for the observations with the mHz QRM. The reference energy band is LE 1–6 keV. The chosen energy bands are (a) 6–9 keV, (b) 9–15 keV, (c) 15–21 keV, (d) 21–27 keV, (e) 27–40 keV, (f) 40–60 keV, and (g) 60–100 keV. The red vertical line marks the centroid frequency of the mHz QRM. The blue points mark the frequency range (ν 0 − FWHM/2, ν 0 + FWHM/2) over which the phase lags of the mHz QRM are averaged. As in Figure 5, the data we used are from all the observations with the mHz QRM.
Paper: An Insight-HXMT View of the mHz Quasi-regular Modulation Phenomenon in the Black Hole X-Ray Binary 4U 1630–47
Authors: Zi-xu Yang, Liang Zhang, Yue Huang, Qingcui Bu, Zhen Zhang, He-Xin Liu, Wei Yu, Peng-Ju Wang, Q. C. Zhao, L. Tao, Jin-Lu Qu, Shu Zhang, Shuang-Nan Zhang, Liming Song, Fangjun Lu, Xuelei Cao, Li Chen, Ce Cai, Zhi Chang, Tianxiang Chen, Yong Chen, Yupeng Chen, Yibao Chen, Weiwei Cui, Guoqiang Ding, Yuanyuan Du, Guanhua Gao, He Gao, Mingyu Ge, Yudong Gu, Ju Guan, Chengcheng Guo, Dawei Han, Jia Huo, Shumei Jia, Weichun Jiang, Jing Jin, Lingda Kong, Bing Li, Gang Li, Wei Li, Xian Li, Xufang Li, Zhengwei Li, Chengkui Li, Lin Lin, Congzhan Liu, Tipei Li, Xiaobo Li, Xiaohua Liang, Jinyuan Liao, Hongwei Liu, Xiaojing Liu, Xuefeng Lu, Qi Luo, Tao Luo, Binyuan Ma, RuiCan Ma, Xiang Ma, Bin Meng, Yi Nang, Jianyin Nie, Ge Ou, Xiaoqin Ren, Na Sai, Xinying Song, Liang Sun, Ying Tan, Youli Tuo, Chen Wang, Wenshuai Wang, Lingjun Wang, Yusa Wang, Jieshuang Wang, Xiangyang Wen, Bobing Wu, Baiyang Wu, Mei Wu, Shuo Xiao, Yupeng Xu, Shaolin Xiong, Sheng Yang, Yanji Yang, Qibin Yi, Qianqing Yin, Yuan You, Bing Zhang, Fan Zhang, Hongmei Zhang, Juan Zhang, Wanchang Zhang, Wei Zhang, Binbin Zhang, Peng Zhang, Yifei Zhang, Yuanhang Zhang, Haisheng Zhao, Xiaofan Zhao, Shijie Zheng, Dengke Zhou
Figure caption: Phase/time lags as a function of photon energy. The reference energy band is LE 1–6 keV. The chosen energy bands are 6–9 keV, 9–15 keV, 15–21 keV, 21–27 keV, 27–40 keV, 40–60 keV, and 60–100 keV. The black points are the phase/time lags of the mHz QRM measured from the frequency-dependent phase-lag spectra by averaging the lags in the QRM frequency range (ν 0 ± FWHM/2, blue points in Figure 6). The orange points are the time lags measured from cross-correlation in the time domain of two different energy band light curves.
Paper: An Insight-HXMT View of the mHz Quasi-regular Modulation Phenomenon in the Black Hole X-Ray Binary 4U 1630–47
Authors: Zi-xu Yang, Liang Zhang, Yue Huang, Qingcui Bu, Zhen Zhang, He-Xin Liu, Wei Yu, Peng-Ju Wang, Q. C. Zhao, L. Tao, Jin-Lu Qu, Shu Zhang, Shuang-Nan Zhang, Liming Song, Fangjun Lu, Xuelei Cao, Li Chen, Ce Cai, Zhi Chang, Tianxiang Chen, Yong Chen, Yupeng Chen, Yibao Chen, Weiwei Cui, Guoqiang Ding, Yuanyuan Du, Guanhua Gao, He Gao, Mingyu Ge, Yudong Gu, Ju Guan, Chengcheng Guo, Dawei Han, Jia Huo, Shumei Jia, Weichun Jiang, Jing Jin, Lingda Kong, Bing Li, Gang Li, Wei Li, Xian Li, Xufang Li, Zhengwei Li, Chengkui Li, Lin Lin, Congzhan Liu, Tipei Li, Xiaobo Li, Xiaohua Liang, Jinyuan Liao, Hongwei Liu, Xiaojing Liu, Xuefeng Lu, Qi Luo, Tao Luo, Binyuan Ma, RuiCan Ma, Xiang Ma, Bin Meng, Yi Nang, Jianyin Nie, Ge Ou, Xiaoqin Ren, Na Sai, Xinying Song, Liang Sun, Ying Tan, Youli Tuo, Chen Wang, Wenshuai Wang, Lingjun Wang, Yusa Wang, Jieshuang Wang, Xiangyang Wen, Bobing Wu, Baiyang Wu, Mei Wu, Shuo Xiao, Yupeng Xu, Shaolin Xiong, Sheng Yang, Yanji Yang, Qibin Yi, Qianqing Yin, Yuan You, Bing Zhang, Fan Zhang, Hongmei Zhang, Juan Zhang, Wanchang Zhang, Wei Zhang, Binbin Zhang, Peng Zhang, Yifei Zhang, Yuanhang Zhang, Haisheng Zhao, Xiaofan Zhao, Shijie Zheng, Dengke Zhou
Figure caption: The best-fitting models and the corresponding residuals to the five spectra with model constant ∗ TBabs ∗ thcomp ∗ diskbb.
Paper: Nonlinear Evolution of Streaming Instabilities in Accreting Protoplanetary Disks
Authors: Chun-Yen Hsu (徐峻彥), Min-Kai Lin (林明楷)
Figure caption: Time evolution of the vertically averaged dust density (left) and radial dust mass flux (right) for the classic SI (run E3eta005am0). Arrows are drawn by inspection and indicate the drift of dust filaments.
Paper: Nonlinear Evolution of Streaming Instabilities in Accreting Protoplanetary Disks
Authors: Chun-Yen Hsu (徐峻彥), Min-Kai Lin (林明楷)
Figure caption: Time evolution of the maximum dust density perturbation in viscous simulations of the AdSI with ﹩\widetilde{\eta }=0﹩ and α  M  = 0.1. The red lines and blue lines corresponds to ϵ = 3 and 0.2, respectively. The solid lines, dashed–dotted lines, and dashed lines corresponds to α visc = 10−8, α visc = 10−7, and α visc = 10−6, respectively. The horizontal dashed–dotted line corresponds to the clumping condition, Equation (25).
Paper: Nonlinear Evolution of Streaming Instabilities in Accreting Protoplanetary Disks
Authors: Chun-Yen Hsu (徐峻彥), Min-Kai Lin (林明楷)
Figure caption: Fraction of the total dust mass with a given radial velocity w  x  (black, left axis) and average dust density associated with a given w  x  (red, right axis), for the classic SI (left panel) and the AdSI (right panel). The vertical, blue dashed line corresponds to the equilibrium drift velocities in each case.
Paper: Nonlinear Evolution of Streaming Instabilities in Accreting Protoplanetary Disks
Authors: Chun-Yen Hsu (徐峻彥), Min-Kai Lin (林明楷)
Figure caption: Same as Figure 9, but for the AdSI (run E3eta0am01).
Paper: Nonlinear Evolution of Streaming Instabilities in Accreting Protoplanetary Disks
Authors: Chun-Yen Hsu (徐峻彥), Min-Kai Lin (林明楷)
Figure caption: Dust density in the inviscid (α visc = 0) and viscous (α visc = 10−7) runs of the AdSI (﹩\epsilon =3,\tilde{\eta }=0,{\alpha }_{M}=0.1﹩).
Paper: Nonlinear Evolution of Streaming Instabilities in Accreting Protoplanetary Disks
Authors: Chun-Yen Hsu (徐峻彥), Min-Kai Lin (林明楷)
Figure caption: Comparison between growth rates of the AdSI computed from linear theory (blue curves) and that measured from numerical simulations (red circles), for fixed ϵ = 3, St = 0.1, ﹩\widetilde{\eta }=0﹩, K  z  = 100, as a function of α  M .
Paper: Nonlinear Evolution of Streaming Instabilities in Accreting Protoplanetary Disks
Authors: Chun-Yen Hsu (徐峻彥), Min-Kai Lin (林明楷)
Figure caption: Same as Figure 13, but for ϵ = 0.2.