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Paper: Natural Generation of Alfvén Waves from Three-dimensional Bursty Interchange Magnetic Reconnection in the Solar Corona
Authors: Liping Yang, Jiansen He, Xueshang Feng, Daniel Verscharen, Fan Guo, Hui Li, Hui Tian, Wenya Li, Fang Shen, Chuanpeng Hou, Mijie Shi, Honghong Wu, Ming Xiong
Figure caption: Observations and 3D modeling of interchange reconnection in the solar corona. (a) Solar Dynamics Observatory/Atmospheric Imaging Assembly 193 Å image of the polar coronal hole on 2018 January 9, showing many bright points and jets. (b) Enlarged view of the jet marked by the blue square in panel (a). (c) 3D view of magnetic field lines and excited Alfvén waves at t = 534.5 s. Here, the colored rods represent magnetic field lines, and the colors denote the values of the velocity component, Vy. The red stars mark possible reconnection sites. (d) Energy spectra of the velocity V (red line) and the magnetic field B (green line), which display power-law profiles. (e) Variations of the velocity component Vz (orange curve) and the Alfvén velocity component −VAy( = −By/ρ0.5) (cyan curve) along the white line in panel (c). (f) The distance–time evolution of Vy along the white line in panel (c), with the red dashed lines showing the propagating speed.
Paper: Natural Generation of Alfvén Waves from Three-dimensional Bursty Interchange Magnetic Reconnection in the Solar Corona
Authors: Liping Yang, Jiansen He, Xueshang Feng, Daniel Verscharen, Fan Guo, Hui Li, Hui Tian, Wenya Li, Fang Shen, Chuanpeng Hou, Mijie Shi, Honghong Wu, Ming Xiong
Figure caption: Development of an Alfvén wave packet in the reconnecting current sheet. (a)–(d) Distributions of the Alfvén velocity component VAy, the velocity component Vy, the discretized y-component of the magnetic tension force (VA·∇)VAy, and the discretized y-component of the total pressure gradient force ﹩-{({\rm{\nabla }}{P}_{t})}_{y}/\rho ﹩ in a subregion of the x−z slice. The blue square highlights the Alfvén wave packet. The black dashed lines represent the magnetic field lines, with arrows denoting the direction of the magnetic field.
Paper: Single-pulse-based Interstellar Scintillation Studies of RRATs
Authors: Zi-wei Wu, Wei-wei Zhu, Zi-yao Fang, Qiu-yang Fu, Ji-guang Lu, Ling-qi Meng, Chen-Chen Miao, Xue-li Miao, Jia-rui Niu, Rukeya Rejiefu, Xun Shi, Chao Wang, Meng-yao Xue, Mao Yuan, You-ling Yue, Chun-feng Zhang, Zhen Zhang, Shi-jun Dang, Yu-lan Liu
Figure caption: Measured correlation coefficients between single-pulse pairs of pulsar J1509+5531 (left panel), the corresponding 2D ACF (middle panel), and secondary spectrum (right panel) with FAST at 1.0–1.5 GHz with frequency resolution of 61 kHz. We select 271 bright single pulses (the peak signal-to-noise ratio ≥ 500) spanning about 26 minutes to do the experiment of single-pulse-based interstellar scintillation. The number of correlation coefficient measurements is larger than 73,000. The time resolution of the time lag of correlation coefficients is the spin period of this pulsar (∼0.74 s). The inverted parabolic arclets are visible. Note that the axis scales of the 2D ACF and secondary spectrum are adjusted to highlight the majority of the details.
Paper: Single-pulse-based Interstellar Scintillation Studies of RRATs
Authors: Zi-wei Wu, Wei-wei Zhu, Zi-yao Fang, Qiu-yang Fu, Ji-guang Lu, Ling-qi Meng, Chen-Chen Miao, Xue-li Miao, Jia-rui Niu, Rukeya Rejiefu, Xun Shi, Chao Wang, Meng-yao Xue, Mao Yuan, You-ling Yue, Chun-feng Zhang, Zhen Zhang, Shi-jun Dang, Yu-lan Liu
Figure caption: The 2D ACFs of four RRATs with FAST. In the two smaller side plots, the gray points are the 1D ACFs at zero frequency and time lag, and the red dashed curves are the best fits from which the scintillation timescale τd and scintillation bandwidth Δνd are derived, respectively.
Paper: Spatially Resolved Oscillations of a Flare Looptop X-Ray Source
Authors: Fanpeng Shi, Alexander Warmuth, Dong Li, Qingmin Zhang, Zongjun Ning, Stefan Purkhart, Song Tan, Frédéric Schuller, Jake A. J. Mitchell
Figure caption: (a) Fit of GBM spectrum using a thermal (“vth”) plus thick-target bremsstrahlung (“thick2”) plus albedo model. The vertical orange lines indicate the energy range used for fit. The fit parameters are also given. (b)–(c) Fits of STIX spectrum using “vth+thin2” and “vth+thick2” model. (d)–(i) Temporal evolution of EM, temperature T, normalized factor/electron flux, spectral indices δ of nonthermal electron and their differences, low-energy cutoffs Ec of nonthermal electrons, and reduced χ2, respectively.
Paper: Spatially Resolved Oscillations of a Flare Looptop X-Ray Source
Authors: Fanpeng Shi, Alexander Warmuth, Dong Li, Qingmin Zhang, Zongjun Ning, Stefan Purkhart, Song Tan, Frédéric Schuller, Jake A. J. Mitchell
Figure caption: (a)–(c) AIA 131 Å image taken at 12:56, EM map, and EM-weighted temperature map, respectively. The reprojection of centroid of looptop X-ray source (4–10 keV) is also overplotted. (d) The best-fit DEM profiles of the cusp (white box of 2.6 × 2.6 Mm2) and background (red box of 2.6 × 2.6 Mm2) regions marked in (a)–(c). The colored rectangles represent the probabilities that MC solutions fall within them. (e) STIX 4–10 keV image reconstructed with VIS_FWDFIT algorithm. The measurements of dimensions of the looptop source are also given. (f)–(g) The diagrams of electron density (in units of 109 cm−3) and nonthermal electron stopping energy (in units of keV).
Paper: Spatially Resolved Oscillations of a Flare Looptop X-Ray Source
Authors: Fanpeng Shi, Alexander Warmuth, Dong Li, Qingmin Zhang, Zongjun Ning, Stefan Purkhart, Song Tan, Frédéric Schuller, Jake A. J. Mitchell
Figure caption: (a) The positions of the STIX 4–10 keV source at different times (color bar) in helioprojective Cartesian coordinates. The orange line is the linear fit of these positions, and the asterisk indicates the starting point. (b) The STIX 4–10 keV counts used for imaging. (c) The temporal evolution of height at STIX 4–10 keV. The slope of linear fit indicates an average rising speed of 7.7 km s−1. (d) The transverse motions of sources. (e)–(h) Similar to (a)–(d), the results for 10–15 keV.
Paper: Spatially Resolved Oscillations of a Flare Looptop X-Ray Source
Authors: Fanpeng Shi, Alexander Warmuth, Dong Li, Qingmin Zhang, Zongjun Ning, Stefan Purkhart, Song Tan, Frédéric Schuller, Jake A. J. Mitchell
Figure caption: (a) The time profiles of detrended intensity and height, and their cross correlation diagrams. The results of STIX 4–10 keV and 10–15 keV are shown in the left and right panels, respectively. (b)–(c) The wavelet analysis of intensity and height, including the local wavelets and the corresponding global power spectra. The 95% significance levels are overplotted.
Paper: Spatially Resolved Oscillations of a Flare Looptop X-Ray Source
Authors: Fanpeng Shi, Alexander Warmuth, Dong Li, Qingmin Zhang, Zongjun Ning, Stefan Purkhart, Song Tan, Frédéric Schuller, Jake A. J. Mitchell
Figure caption: (a) The relative locations of the SolO, the Sun, and near-Earth observatories (GOES, SDO, Fermi). (b)–(d) FSI 174 Å, AIA 1600 Å, and AIA 131 Å images taken at 13:02, respectively. The solar limbs seen from FSI and AIA are also overplotted. (e)–(g) The lightcurves of GOES, GBM, and STIX from 12:45 to 13:30.
Paper: Spatially Resolved Oscillations of a Flare Looptop X-Ray Source
Authors: Fanpeng Shi, Alexander Warmuth, Dong Li, Qingmin Zhang, Zongjun Ning, Stefan Purkhart, Song Tan, Frédéric Schuller, Jake A. J. Mitchell
Figure caption: Schematic diagram of the possible origin of double periods in oscillations. (Left) The periodic signals of 2 minutes (blue) and relatively weaker 1 minutes (orange), and the synthetic signal (green). (Right) The sketch of plasmoids (2 and 1 minute periods) at three different times.
Paper: FAST Discovery of a Gas-rich and Ultrafaint Dwarf Galaxy: KK153
Authors: Jin-Long Xu, Ming Zhu, Nai-Ping Yu, Chuan-Peng Zhang, Xiao-Lan Liu, Mei Ai, Peng Jiang
Figure caption: (a) H I column-density map of KK153 from the FAST observation shown in white contours overlaid on the DESI-red, green, and blue (RGB; g, r, z) image in color scale. The white contours begin at 4.2 × 1017 cm−2 (3σ) in steps of 2.0 × 1018 cm−2. (b) The zoomed-in DESI-RGB image of KK153.
Paper: FAST Discovery of a Gas-rich and Ultrafaint Dwarf Galaxy: KK153
Authors: Jin-Long Xu, Ming Zhu, Nai-Ping Yu, Chuan-Peng Zhang, Xiao-Lan Liu, Mei Ai, Peng Jiang
Figure caption: (a) Velocity-field map of KK153 in color scale overlaid with its H I column-density map in black contours. The black contours begin at 4.2 × 1017 cm−2 in steps of 2.0 × 1018 cm−2. (b), (c) Position–velocity (PV) diagrams of the observed data in color scale overlaid with black contours. The black contours begin at 3σ (3.0 mJy beam−1) in steps of 3σ. The cutting direction of the PV diagrams is indicated by the blue arrow in panel (a).
Paper: FAST Discovery of a Gas-rich and Ultrafaint Dwarf Galaxy: KK153
Authors: Jin-Long Xu, Ming Zhu, Nai-Ping Yu, Chuan-Peng Zhang, Xiao-Lan Liu, Mei Ai, Peng Jiang
Figure caption: Baryonic Tully–Fisher relation (BTFR). The red dashed line represents a best-fit relation ﹩\mathrm{log}({M}_{\mathrm{bar}})=a+b\times \mathrm{log}({V}_{\mathrm{rot}})﹩, where a = 1.61 ± 0.18 and b = 4.04 ± 0.09. The gas-dominated galaxies are marked by black points (S. S. McGaugh & J. M. Schombert 2015). The black dashed line marks the rotation velocity of KK153, while the green shaded area represents the range of its baryonic mass.
Paper: FAST Discovery of a Gas-rich and Ultrafaint Dwarf Galaxy: KK153
Authors: Jin-Long Xu, Ming Zhu, Nai-Ping Yu, Chuan-Peng Zhang, Xiao-Lan Liu, Mei Ai, Peng Jiang
Figure caption: Left panel: the distribution of DESI g – r color in each pixel for KK153. Right panel: the WISE W1-band emission of KK153.
Paper: FAST Discovery of a Gas-rich and Ultrafaint Dwarf Galaxy: KK153
Authors: Jin-Long Xu, Ming Zhu, Nai-Ping Yu, Chuan-Peng Zhang, Xiao-Lan Liu, Mei Ai, Peng Jiang
Figure caption: Global H I profile of KK153 shown by a black line. The green line indicates the BusyFit fitting result, while the red and blue lines represent the double Gaussian fitting results. The residual after the Gaussian fitting is represented by a red dashed line.
Paper: Spatially Resolved Oscillations of a Flare Looptop X-Ray Source
Authors: Fanpeng Shi, Alexander Warmuth, Dong Li, Qingmin Zhang, Zongjun Ning, Stefan Purkhart, Song Tan, Frédéric Schuller, Jake A. J. Mitchell
Figure caption: (a) The time profiles of detrended normalized factor/electron flux and spectral index δ, and their cross correlation diagrams. (b)–(e) The wavelet analysis of detrended curves, including the local wavelets and the corresponding global power spectra. The 95% significance levels are overplotted.
Paper: How to Escape from a Trap: Outcomes of Repeated Black Hole Mergers in Active Galactic Nuclei
Authors: Shmuel Gilbaum, Evgeni Grishin, Nicholas C. Stone, Ilya Mandel
Figure caption: Normalized distributions of realignment times TRA for a m• = 10M⊙ object in the outermost migration trap, shown as a function of SMBH mass M, fixing the AGN Eddington ratio ﹩\dot{M}/{\dot{M}}_{{\rm{Edd}}}=0.1﹩ and α = 0.1. Color coding represents the probability density for different TRA assuming a mass ratio q = 1, spin magnitude of χ1,2 = 0.7 for both black holes, and random spin misalignment of up to 30° with respect to the angular momentum of the AGN disk. The green dotted line represents upper limits on observed AGN lifetimes (Appendix A.4) at redshift z = 0.1. The orange and blue dashed lines represent the approximate maximum (minimum) times for a merger due to 2 + 1 scattering against 1 (﹩{N}_{{\rm{\max }}}﹩) BHs. The violet solid line represents the local dynamical time at the trap. The pink (gray) dotted line is the mass-doubling time of an embedded object via Eddington (Bondi–Hoyle–Lyttleton) rate accretion. The dashed–dotted brown shows the time for a sufficiently heavy BH to escape the entire trap region via Type II migration. The yellow dotted line represents an example timescale for the influx of black holes to the trap (1/Ṅ).
Paper: How to Escape from a Trap: Outcomes of Repeated Black Hole Mergers in Active Galactic Nuclei
Authors: Shmuel Gilbaum, Evgeni Grishin, Nicholas C. Stone, Ilya Mandel
Figure caption: The minimum mass (Mgap) for escaping the migration trap via gap opening (the maximum of gap-opening masses between the antitrap and the trap) for an α = 0.1 disk, shown in color coding as a function of SMBH mass M and AGN Eddington ratio ﹩\dot{M}/{\dot{M}}_{{\rm{Edd}}}﹩. The solid contour lines highlight individual values of Mgap as labeled. The dashed contour lines represent the AGN luminosity L, assuming a radiative efficiency η = 0.1. Hierarchical growth in traps only occurs in a relatively narrow range of AGN luminosities, for 1043.5 erg s−1 ≲ L ≲ 1045.5 erg s−1. At higher luminosities, the traps fail to exist (E. Grishin et al. 2024); at lower luminosities, gaps open too easily to retain merger products in the traps. The maximum value we find is Mgap ≈ 150M⊙, though larger masses arise for lower α (see Appendix B and Figure 8).
Paper: How to Escape from a Trap: Outcomes of Repeated Black Hole Mergers in Active Galactic Nuclei
Authors: Shmuel Gilbaum, Evgeni Grishin, Nicholas C. Stone, Ilya Mandel
Figure caption: The color-coded minimum mass for opening a gap, Mgap, computed for an ensemble of α = 0.01 AGN disks with varying central mass M. Notation is the same as in Figure 3 (where α = 0.1 was used). One notable change from the high-α case is that here, we see regions (M ∼ 5 × 107M⊙) where “gap-closing” traps exist, i.e., where Mgap increases at radii beneath the linear trap.
Paper: How to Escape from a Trap: Outcomes of Repeated Black Hole Mergers in Active Galactic Nuclei
Authors: Shmuel Gilbaum, Evgeni Grishin, Nicholas C. Stone, Ilya Mandel
Figure caption: The minimum mass for escaping the migration trap via gap opening (i.e., the maximum gap-opening mass Mgap between the antitrap and trap) for α = 0.01. Notation is the same as in Figure 4 (where α = 0.1 was used). The higher-Σ disks shown here feature, in some parts of parameter space, much larger maximum Mgap values, peaking at ∼4 × 103M⊙ for high M and low Eddington ratio ﹩\dot{M}/{\dot{M}}_{{\rm{Edd}}}﹩.
Paper: How to Escape from a Trap: Outcomes of Repeated Black Hole Mergers in Active Galactic Nuclei
Authors: Shmuel Gilbaum, Evgeni Grishin, Nicholas C. Stone, Ilya Mandel
Figure caption: The color-coded minimum mass for opening a gap, Mgap, plotted in the 2D parameter space of SMBH mass M and radial location R/Rg. This plot takes the Eddington ratio ﹩\dot{M}/{\dot{M}}_{{\rm{Edd}}}=0.1﹩ and α = 0.1. Labeled contours highlight particular values of Mgap. The blue (cyan) dotted lines indicate the trap (antitrap) locations. At low SMBH masses, even small stellar mass BHs can open gaps at all radii, making hierarchical growth unlikely in migration traps.
Paper: How to Escape from a Trap: Outcomes of Repeated Black Hole Mergers in Active Galactic Nuclei
Authors: Shmuel Gilbaum, Evgeni Grishin, Nicholas C. Stone, Ilya Mandel
Figure caption: The radial locations Rtrap of migration traps and antitraps as a function of SMBH mass M, for Eddington ratio ﹩\dot{M}/{\dot{M}}_{{\rm{Edd}}}=0.1﹩ and the perturber BH mass m• = 10M⊙. Blue (cyan) points represent the traps (antitraps) for α = 0.1, and red (orange) points represent α = 0.01. The two dashed lines show the location where the Toomre parameter QT = 1 for each α. For the α = 0.01 case, there are some masses M that produce two traps; at the highest M values, no traps exist (E. Grishin et al. 2024).
Paper: How to Escape from a Trap: Outcomes of Repeated Black Hole Mergers in Active Galactic Nuclei
Authors: Shmuel Gilbaum, Evgeni Grishin, Nicholas C. Stone, Ilya Mandel
Figure caption: Normalized distributions of inclination and eccentricity (from left to right in each panel) for BBH mergers at each radius for different conditions. The left panel (a) shows results for both black holes with dimensionless spin magnitude χ = 0.7. The right panel shows results for one black hole (the heavier one) with dimensionless spin χ = 0.7, and the second black hole with weaker spin χ = 0.1. In both panels the top (bottom) row shows a BBH with mass ratio q = 0.1 (q = 1). The white dashed line in the eccentricity panels corresponds to e = 1; all simulations above the line escape the SMBH system due to the kick. In the inclination panels, the escaped cases are shown to have an inclination of exactly π/2 (note there is a gap between that and the actually highest inclination).
Paper: How to Escape from a Trap: Outcomes of Repeated Black Hole Mergers in Active Galactic Nuclei
Authors: Shmuel Gilbaum, Evgeni Grishin, Nicholas C. Stone, Ilya Mandel
Figure caption: Timescales and realignment times for α = 0.01. Notation is the same as in Figure 2 (in which α = 0.1 was used). In the higher-Σ conditions of this low-α disk, we see much shorter realignment and Type II escape times.
Paper: Natural Generation of Alfvén Waves from Three-dimensional Bursty Interchange Magnetic Reconnection in the Solar Corona
Authors: Liping Yang, Jiansen He, Xueshang Feng, Daniel Verscharen, Fan Guo, Hui Li, Hui Tian, Wenya Li, Fang Shen, Chuanpeng Hou, Mijie Shi, Honghong Wu, Ming Xiong
Figure caption: Properties of the Alfvén waves launched by interchange reconnection in the solar corona. (a) Wave energy flux Fwy in the x–z slice at t = 665.0 s. Gray dashed lines represent magnetic field lines, with arrows indicating the field direction. (b) The rms values of Vy in the x–z slice. (c)–(e) Temporal variations of the perturbed velocity components (δVx and δVy, black lines); the negative perturbed Alfvén velocity components (−​​​​​​δVAx and −δVAyAy, blue lines); δVz/Cs, with Cs being sonic speed and calculated by the mean thermal pressure and the mean density (black line); and δρ/ρ0, with ρ0 being the mean density (blue line) at the point of x = 19.5 Mm, y = 40.0 Mm, and z = 25.0 Mm (the red dot in panel (a)) on the wave path. (f)–(g) Spectra of the angle between the wavevector k and the local mean magnetic field B0 (﹩{\theta }_{{\boldsymbol{k}},{{\boldsymbol{B}}}_{{0}}}﹩, f) and the angle between the perturbed magnetic field δB and B0 (﹩{\theta }_{\delta {\boldsymbol{B}},{{\boldsymbol{B}}}_{{\bf{0}}}}﹩, g). (h) The sense of magnetic polarization about B0 with the values of −1 and +1 denoting the left-hand and right-hand circular polarization. (i) Ellipticity of the polarization, where 0 represents linear and 1 represents circular polarization. The black curve in panels (f)–(i) shows the profile of the cone of influence of the wavelet transform.
Paper: Is the Spin of the Black Hole in GX 339–4 Negative?
Authors: Andrzej A. Zdziarski, Srimanta Banerjee, Michał Szanecki, Ranjeev Misra, Gulab Dewangan
Figure caption: The NICER (black) and NuSTAR (blue and red) unfolded spectra (top panels) and data-to-model ratios (bottom panels) for the joint fit with model 3 (see Table 2) to the data from (a) 2020 and (b) 2021. The spectra are normalized to NuSTAR A. The model is of Equation (2) with disk = slimbh and the atmospheric spectra. The total model spectra and the unabsorbed one are shown by the solid black and blue curves, respectively. The unabsorbed disk emission, scattering alone, and reflection are shown by the magenta, green, and red curves, respectively.
Paper: Is the Spin of the Black Hole in GX 339–4 Negative?
Authors: Andrzej A. Zdziarski, Srimanta Banerjee, Michał Szanecki, Ranjeev Misra, Gulab Dewangan
Figure caption: Correlations between the main parameters calculated by MCMC for model 3. The median values and the 90% uncertainties are shown by the middle and surrounding dashed lines, respectively. The corresponding numerical values are given by the posterior distributions, which agree well with those in Table 2 (χ2-based).
Paper: Petrogenesis of Chang’e-6 Basalts and Implication for the Young Volcanism on the Lunar Farside
Authors: Chengxiang Yin, Jian Chen, Xiaohui Fu, Haijun Cao, Xuejin Lu, Yiheng Liu, Jin Li, Siyue Chi, Xiaojia Zeng, Zongcheng Ling
Figure caption: Reverse fractional crystallization of CE-6 basalt to estimate the primitive magma compositions. The CPX of 0, 10, and 20 mass% as well as olivine were incrementally added back into the bulk composition of CE-6 basalt. The intersection of reversed fractional crystallization trend and lunar mantle melting path (lunar mantle partial melt, B. Su et al. 2022) defines CE-6 basalt primitive magma (MgO ∼ 15 wt%).
Paper: Petrogenesis of Chang’e-6 Basalts and Implication for the Young Volcanism on the Lunar Farside
Authors: Chengxiang Yin, Jian Chen, Xiaohui Fu, Haijun Cao, Xuejin Lu, Yiheng Liu, Jin Li, Siyue Chi, Xiaojia Zeng, Zongcheng Ling
Figure caption: Bulk composition of CE-6 basalt and comparison with other lunar samples. (a) FeO-TiO2 and (b) Al2O3-TiO2 plots. The CE-3/CE-5/CE-6 soils data are from Z. Ling et al. (2015), C. Li et al. (2022), K. Zong et al. (2022), and C. Li et al. (2024), respectively. The data of CE-5 basalt and CE-6 subophitic basalt are sourced from H.-C. Tian et al. (2021) and C. Li et al. (2024), respectively. The data of Apollo and Luna basalts are derived from the mare basalts database compiled by Clive Neal (https://www3.nd.edu/~cneal/Lunar-L/Mare-Basalt-Database.xls).
Paper: Petrogenesis of Chang’e-6 Basalts and Implication for the Young Volcanism on the Lunar Farside
Authors: Chengxiang Yin, Jian Chen, Xiaohui Fu, Haijun Cao, Xuejin Lu, Yiheng Liu, Jin Li, Siyue Chi, Xiaojia Zeng, Zongcheng Ling
Figure caption: REE pattern of CE-6 basalt primary parent melt. (a) Comparison with CE-5 (C. Li et al. 2022; K. Zong et al. 2022)/CE-6 soils (C. Li et al. 2024), CE-5 basalt, and CE-5 basalt primary parent melt (H.-C. Tian et al. 2021). The REE contents of CE-6 basalt primary parent melt were estimated based on the average composition of Mg-rich pyroxene (blue line) and using partition coefficients reported by L. Yao et al. (2012). The Mare/KREEP basalt range was adapted from K. H. Joy et al. (2011). (b) Comparison with primary parent melts of Apollo basalts (L. J. Hallis et al. 2014 and references therein) and CE-5 basalt (H.-C. Tian et al. 2021).
Paper: Petrogenesis of Chang’e-6 Basalts and Implication for the Young Volcanism on the Lunar Farside
Authors: Chengxiang Yin, Jian Chen, Xiaohui Fu, Haijun Cao, Xuejin Lu, Yiheng Liu, Jin Li, Siyue Chi, Xiaojia Zeng, Zongcheng Ling
Figure caption: Fractional crystallization sequence of CE-6 basalt primitive magma with 20% CPX added at a changed pressure from 1 kbar to 1 bar. The magma in a chamber beneath the Apollo floor began to crystallize at a pressure of 1 kbar. After the 40%–50% crystallization, the melts ascended and eventually erupted onto the lunar surface (the pressure is assumed to be about 1 bar).
Paper: Petrogenesis of Chang’e-6 Basalts and Implication for the Young Volcanism on the Lunar Farside
Authors: Chengxiang Yin, Jian Chen, Xiaohui Fu, Haijun Cao, Xuejin Lu, Yiheng Liu, Jin Li, Siyue Chi, Xiaojia Zeng, Zongcheng Ling
Figure caption: Floor-fractured craters in large-scale basins on the lunar farside. Their locations are shown in Figure 5. The blue-filled areas represent mare basalt deposits, and the cyan dashed lines depict the basin rings. White arrows indicate typical floor-fractured craters. Lunar Reconnaissance Orbiter Camera Wide Angle Camera image (M. S. Robinson et al. 2010) was employed here.
Paper: Petrogenesis of Chang’e-6 Basalts and Implication for the Young Volcanism on the Lunar Farside
Authors: Chengxiang Yin, Jian Chen, Xiaohui Fu, Haijun Cao, Xuejin Lu, Yiheng Liu, Jin Li, Siyue Chi, Xiaojia Zeng, Zongcheng Ling
Figure caption: Fractional crystallization trend line of the CE-6 basalt primitive magma, obtained by adding olivine following the incorporation of 20% CPX (i.e., 20% CPX + Ol), under different pressure conditions. Except for the 5 kbar pressure, the fractional crystallization trend lines under other pressure conditions (i.e., 1 bar, 1 kbar, and 1 kbar_1 bar) nearly overlap. The 1 kbar_1 bar refers to a changed pressure from 1 kbar to 1 bar after 45% fractional crystallization.