adsabs/AstroCLIMB huggingface dataset:
Paper: ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Deriving Inclination Angle and Velocity of the Protostellar Jets from Their SiO Knots
Authors: Kai-Syun Jhan, Chin-Fei Lee, Doug Johnstone, Tie Liu, Sheng-Yuan Liu, Naomi Hirano, Ken'ichi Tatematsu, Somnath Dutta, Anthony Moraghan, Hsien Shang, Jeong-Eun Lee, Shanghuo Li, Chun-Fan Liu, Shih-Ying Hsu, Woojin Kwon, Dipen Sahu, Xun-Chuan Liu, Kee-Tae Kim, Qiuyi Luo, Sheng-Li Qin, Patricio Sanhueza, Leonardo Bronfman, Zhang Qizhou, David Eden, Alessio Traficante, Chang Won Lee
Figure caption: PV diagrams of the jets along the jet axis in SiO. The width of the green line segment denotes the observed radial sideways-ejection velocity (ΔV obs) for each source, and the dotted line denotes the observed radial jet velocity (V obs). The contour levels start at 3σ with a step of 3σ, and σ are ∼0.002, 0.002, 0.002, and 0.0019 Jy beam−1 in panels (a) to (d), respectively.
Paper: ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Deriving Inclination Angle and Velocity of the Protostellar Jets from Their SiO Knots
Authors: Kai-Syun Jhan, Chin-Fei Lee, Doug Johnstone, Tie Liu, Sheng-Yuan Liu, Naomi Hirano, Ken'ichi Tatematsu, Somnath Dutta, Anthony Moraghan, Hsien Shang, Jeong-Eun Lee, Shanghuo Li, Chun-Fan Liu, Shih-Ying Hsu, Woojin Kwon, Dipen Sahu, Xun-Chuan Liu, Kee-Tae Kim, Qiuyi Luo, Sheng-Li Qin, Patricio Sanhueza, Leonardo Bronfman, Zhang Qizhou, David Eden, Alessio Traficante, Chang Won Lee
Figure caption: PV diagrams cut perpendicular to the jet axis going through the sources’ center for four sources (G209, G205, G203, and G191) in C18O, centered at the source position. The contour levels start at 3σ with a step of 3σ, and σ are ∼0.003, 0.003, 0.003, and 0.003 Jy beam−1 in panels (a) to (d), respectively. The vertical dashed line indicates the systemic velocity for each source.
Paper: Quasi-periodic Accelerations of Energetic Particles during a Solar Flare
Authors: Dong Li, Wei Chen
Figure caption: Imaging observations of the X4.8 flare with an FOV of ∼100″ × 100″. The background images are measured by RHESSI 50–100 keV (a), NoRH 17 GHz (b), SOHO/MDI (c), and TRACE 195 Å (d), respectively. The overlaid contours represent the HXR and radio emissions derived from RHESSI 50–100 keV (yellow) and 100–300 keV (red), as well as NoRP 17 GHz (orange) and 34 GHz (cyan). Their levels are set at 30%, 60%, and 90%. The circles represent the source locations (see Hurford et al. 2003; Lin et al. 2003) of RHESSI 300–500 keV (magenta), 700–1400 keV (green), and 2218–2228 keV (gold).
Paper: Quasi-periodic Accelerations of Energetic Particles during a Solar Flare
Authors: Dong Li, Wei Chen
Figure caption: (a1)–(a3) Flare fluxes normalized to their maximum values in the γ-ray line and continuum emissions observed by RHESSI (black); the overlaid cyan lines are their slow-varying trends. (b1)–(b3) Detrended light curves normalized to their maximum slow-varying trends. (c1)–(c3) Morlet wavelet power spectra. The magenta contours indicate a significance level of 99.9%.
Paper: Quasi-periodic Accelerations of Energetic Particles during a Solar Flare
Authors: Dong Li, Wei Chen
Figure caption: Similar to Figure 2, but for HXR and radio light curves in the energy range of RHESSI 50–100 keV and at frequencies of NoRP 17 and 80 GHz.
Paper: Quasi-periodic Accelerations of Energetic Particles during a Solar Flare
Authors: Dong Li, Wei Chen
Figure caption: Wavelet amplitude spectra corresponding to the detrended time profiles seen in multiple wavelengths. The magenta contours represent the 99.9% significance level, and the color background indicates the signal variations in time and periods.
Paper: Is the Black-widow Pulsar PSR J1555–2908 in a Hierarchical Triple System?
Authors: L. Nieder, M. Kerr, C. J. Clark, P. Bruel, H. T. Cromartie, S. M. Ransom, P. S. Ray
Figure caption: Measured values of the timing noise power P tn and spectral index Γtn from NANOGrav (blue circles) and the PPTA (orange squares). 1σ uncertainties for the PPTA pulsars are taken from Table 1 by Goncharov et al. (2021). The addition of Γtn to the abscissa converts the power normalization from a frequency of f = 1 yr−1 to f = 0.1 yr−1. The measured value for PSR J1555−2908 (this work) is depicted with a green star. Pulsars with strong timing noise are labeled.
Paper: Is the Black-widow Pulsar PSR J1555–2908 in a Hierarchical Triple System?
Authors: L. Nieder, M. Kerr, C. J. Clark, P. Bruel, H. T. Cromartie, S. M. Ransom, P. S. Ray
Figure caption: Mass–mass diagram where lines show the potential outer companion mass for different inclination angles (measured with respect to line of sight to Earth) and total masses of the inner binary system. For comparison, the masses of the Moon, Mercury, and Mars are indicated by the dashed lines. The dotted line and the gray area mark the most likely value for M p + M i = 1.73 M ⊙ and the associated 95% range from optical modeling (Kennedy et al. 2022).
Paper: On the Single-event-based Identification of Primordial Black Hole Mergers at Cosmological Distances
Authors: Ken K. Y. Ng, Shiqi Chen, Boris Goncharov, Ulyana Dupletsa, Ssohrab Borhanian, Marica Branchesi, Jan Harms, Michele Maggiore, B. S. Sathyaprakash, Salvatore Vitale
Figure caption: Redshift posteriors (offset by the true values) for sources with (M tot, q, ι) = (40M ⊙, 1, π/6) at five different redshifts observed by CE–ET (red) and CE–CES–ET (blue). The solid horizontal lines show the 95% credible intervals, whereas the dashed lines mark z true.
Paper: On the Single-event-based Identification of Primordial Black Hole Mergers at Cosmological Distances
Authors: Ken K. Y. Ng, Shiqi Chen, Boris Goncharov, Ulyana Dupletsa, Ssohrab Borhanian, Marica Branchesi, Jan Harms, Michele Maggiore, B. S. Sathyaprakash, Salvatore Vitale
Figure caption: Posteriors of the system (M tot, q, ι, z) = (40M ⊙, 1, π/3, 40), using p tot(z) evaluated at ﹩{f}_{\mathrm{III}}^{\mathrm{PBH}}=100﹩ (blue), 10 (orange), 1 (green), 0.1 (red), and 0.01 (purple). The black solid line shows the default posterior. The black dashed line indicates z true = 40, and the gray area indicates the astrophysical region z < z crit.
Paper: On the Single-event-based Identification of Primordial Black Hole Mergers at Cosmological Distances
Authors: Ken K. Y. Ng, Shiqi Chen, Boris Goncharov, Ulyana Dupletsa, Ssohrab Borhanian, Marica Branchesi, Jan Harms, Michele Maggiore, B. S. Sathyaprakash, Salvatore Vitale
Figure caption: Prior based on the mixture model p tot (solid lines), ranging from ﹩{f}_{\mathrm{III}}^{\mathrm{PBH}}=100﹩ (blue), 10 (orange), 1 (green), 0.1 (red), and 0.01 (purple). The dashed lines and dashed–dotted lines represent the individual contribution from PBH mergers and Population III BBH mergers (which are truncated at z crit), respectively.
Paper: On the Single-event-based Identification of Primordial Black Hole Mergers at Cosmological Distances
Authors: Ken K. Y. Ng, Shiqi Chen, Boris Goncharov, Ulyana Dupletsa, Ssohrab Borhanian, Marica Branchesi, Jan Harms, Michele Maggiore, B. S. Sathyaprakash, Salvatore Vitale
Figure caption: Redshift posteriors for sources with (q, ι, z) = (1, 0, 40) at four different total masses observed by CE–ET (red) and CE–CES–ET (blue). The solid horizontal lines show the 95% credible intervals, whereas the dashed line marks z true. Only sources with S/N ≥ 12 are included.
Paper: Ellipsars: Ring-like Explosions from Flattened Stars
Authors: Marcus DuPont, Andrew MacFadyen, Jonathan Zrake
Figure caption: Top: the cumulative distribution of the isotropic-equivalent kinetic energy E  k,iso(>Γβ, θ), as a function of the polar angle θ, for representative values of Γβ. The small axes at the top show E  k,iso(>0, θ), i.e., the total isotropic-equivalent kinetic energy as a function of polar angle. The total energy in the domain, above each of the Γβ cutoffs 0.5, 1, 2, and 10, is 1.6 × 1049 erg, 1.75 × 1048 erg, 1.8 × 1047 erg, and 3.0 × 1045 erg, respectively. Bottom: the cumulative distribution of isotropic-equivalent mass M iso(>Γβ, θ), as a function of θ, for representative values of Γβ. The secondary vertical axis at the right shows the nominal deceleration radius r decl. (Equation (5)) corresponding to the mass scale at the left, when A * has the fiducial value of 0.1.
Paper: Ellipsars: Ring-like Explosions from Flattened Stars
Authors: Marcus DuPont, Andrew MacFadyen, Jonathan Zrake
Figure caption: The cumulative distributions of kinetic energy, E  k ( > Γβ), for a suite of explosions with energies between 1051 erg and 1054 erg and oblateness magnitudes ε = 0, 0.05, and 0.2. These distributions were recorded at times when the gas is approximately ballistic, from top to bottom at times 93, 35, 22, 12, and 20 s post-explosion. For all but the largest explosion energy, stars with 5% flattening (ε = 0.05) produce faster ejecta than their spherical counterparts. In general, the spherical star ε = 0 and the overflattened star ε = 0.2 produces less relativistic material than the optimally flattened star (ε = 0.05).
Paper: Ellipsars: Ring-like Explosions from Flattened Stars
Authors: Marcus DuPont, Andrew MacFadyen, Jonathan Zrake
Figure caption: The pressure and four-velocity at t = 93 s showing a cross section (r–θ slice) of the explosion dynamics. The expanding mildly relativistic ring, seen also in the expanded wings, is produced at the equator by the collision of expanding lobes propagating from the poles during a ﹩{E}_{\exp }={10}^{51}\,\mathrm{erg}﹩ point explosion in an oblate star with ε = 0.05. The dashed orange ellipse shows the original size and shape of the progenitor. In the right wing, we see a steep pressure gradient point in the ﹩+\hat{r}﹩ direction, which is the main driver behind the equatorial flow. The left wing shows that the ring expands radially outward with a mildly relativistic speed of Γβ ∼ 0.5.
Paper: Ellipsars: Ring-like Explosions from Flattened Stars
Authors: Marcus DuPont, Andrew MacFadyen, Jonathan Zrake
Figure caption: The dynamical evolution of a 5 × 1052 erg explosion within a 5% flattened progenitor star (shown as the elliptical dashed line with semimajor axis ∼4.5 × 1010 cm.) We first see the deformed prolate shock approach the poles in panel (a). In panel (b), the lobe shocks have spread sideways toward an impending collision point in the equatorial plane. In panel (c), the lobe shocks collide and force material radially outward, forming an expanding relativistic ring.
Paper: Quasi-periodic Accelerations of Energetic Particles during a Solar Flare
Authors: Dong Li, Wei Chen
Figure caption: (a) Radio dynamic spectrum measured by Wind/Waves. The overplotted light curve is recorded by GOES 1–8 Å from 00:10 UT to 01:40 UT. The vertical orange lines mark the start and peak times of the X4.8 flare. (b) Normalized HXR and γ-ray fluxes between 00:25 UT and 00:33 UT observed by RHESSI in energy ranges of 50–100 keV (black), 100–300 keV (red), 300–500 keV (magenta), 700–1400 keV (green), and 2200–2300 keV (blue). (c) Normalized radio fluxes during 00:25–00:33 UT measured by NoRP at frequencies of 17 GHz (black), 35 GHz (cyan), and 80 GHz (pink).
Paper: On the Connection between Supermassive Black Holes and Galaxy Growth in the Reionization Epoch
Authors: Junyao Li, John D. Silverman, Takuma Izumi, Wanqiu He, Masayuki Akiyama, Kohei Inayoshi, Yoshiki Matsuoka, Masafusa Onoue, Yoshiki Toba
Figure caption: Top: predicted evolution of the growth of SMBHs and their host galaxies over the next min(t del, 100) Myr. The dashed arrows represent the evolution vectors assuming the AGN duty cycle derived from the Type 1 BHMF, while the solid arrows show the evolution vectors after correcting the duty cycle for Type 2 AGNs. Two objects with upper limits in SFR are shown as black (gray) arrows. The adopted duty cycle–﹩{{ \mathcal M }}_{\mathrm{BH}}﹩ relations are shown in the inset. The blue and orange arrows show the possible evolution pathways for overly massive quasars. The black dashed line and the shaded region represent the local HR04 relation and its scatter. Bottom: the intersection angle as a function of offset. Each quasar is color-coded by their BH masses. Two objects with upper limits in SFR are marked by blue arrows. The dashed line at θ = 48° represents the slope of the local relation.
Paper: On the Connection between Supermassive Black Holes and Galaxy Growth in the Reionization Epoch
Authors: Junyao Li, John D. Silverman, Takuma Izumi, Wanqiu He, Masayuki Akiyama, Kohei Inayoshi, Yoshiki Matsuoka, Masafusa Onoue, Yoshiki Toba
Figure caption: The ﹩{{ \mathcal M }}_{\mathrm{BH}}\mbox{--}{{ \mathcal M }}_{\star }﹩ distribution at z ∼ 6. The individual points and the red contours (1σ–2σ levels) show the observed quasars color-coded by their M 1450. The blue contours (1σ–3σ levels) show the mock AGN sample, which mimics the selection function and measurement uncertainties of the observations (i.e., Mock-Q) assuming β = 0.6. The average ﹩{{ \mathcal M }}_{\mathrm{BH}}\mbox{--}{{ \mathcal M }}_{\star }﹩ relations of the mock AGN samples (incorporating observational biases) using β = 0.0, 0.6, and 1.0 are plotted as dotted, solid, and dashed blue curves, respectively. The local HR04 relation and its scatter are shown as a black dashed line and a gray shaded region.
Paper: On the Connection between Supermassive Black Holes and Galaxy Growth in the Reionization Epoch
Authors: Junyao Li, John D. Silverman, Takuma Izumi, Wanqiu He, Masayuki Akiyama, Kohei Inayoshi, Yoshiki Matsuoka, Masafusa Onoue, Yoshiki Toba
Figure caption: Parameter distributions of the mock AGN sample. The full mock sample is shown in blue with the contours representing the 1σ–5σ levels. The mock sample matching in M 1450 with the observed z ∼ 6 quasars is shown in red with the contours representing the 1σ–3σ levels.
Paper: On the Connection between Supermassive Black Holes and Galaxy Growth in the Reionization Epoch
Authors: Junyao Li, John D. Silverman, Takuma Izumi, Wanqiu He, Masayuki Akiyama, Kohei Inayoshi, Yoshiki Matsuoka, Masafusa Onoue, Yoshiki Toba
Figure caption: Left: estimating stellar masses of z ∼ 6 quasars by subtracting the expected molecular gas masses (inset histogram) from their dynamical masses. Quasars are plotted as stars color-coded by their M 1450. The blue curve shows the ﹩{{ \mathcal M }}_{\star }﹩–﹩{{ \mathcal M }}_{\mathrm{dyn}}﹩ relation derived from the ﹩{{ \mathcal M }}_{\mathrm{gas}}﹩/﹩{{ \mathcal M }}_{\star }﹩ vs. ﹩{{ \mathcal M }}_{\star }﹩ relation given by Tacconi et al. (2018). The black dashed line shows the one-to-one relation. Right: the SFR–﹩{{ \mathcal M }}_{\star }﹩ plane of our quasars compared to the Speagle et al. (2014) MS relation at z ∼ 6. Two objects with upper limits in SFR are marked by red arrows.
Paper: On the Connection between Supermassive Black Holes and Galaxy Growth in the Reionization Epoch
Authors: Junyao Li, John D. Silverman, Takuma Izumi, Wanqiu He, Masayuki Akiyama, Kohei Inayoshi, Yoshiki Matsuoka, Masafusa Onoue, Yoshiki Toba
Figure caption: Constraining the evolution factor γ and the intrinsic scatter σ  μ  based on a specific model (β = 0.6). The contours represent the 1σ–3σ confidence regions of the posterior probability distribution. The histograms are the marginalized posterior distributions. The star indicates the posterior median and its 1σ error.
Paper: Enhanced Star Formation Activity of Extreme Jellyfish Galaxies in Massive Clusters and the Role of Ram Pressure Stripping
Authors: Jeong Hwan Lee, Myung Gyoon Lee, Jae Yeon Mun, Brian S. Cho, Jisu Kang
Figure caption: Projected phase-space diagrams of our sample (star symbols), the GASP jellyfish galaxies (circles), the A901/2 sample (RO19; diamonds), and the A1758N sample (EK19; triangles). We normalize clustercentric distance (R cl) and absolute relative velocity (∣v los∣) with cluster virial radius (R 200) and velocity dispersion (σ  v,cl), respectively. All the data are color-coded by total SFR (left) and tail SFR (right). The color bars on the top denote the logarithmic scale of each SFR, showing the three categories of star formation activity: “weak,” “moderate,” and “strong.” Gray dashed lines represent a boundary between the virialized region and the recent infall region (Jaffé et al. 2015). We divide the whole sample into two categories by JClass from the GASP studies (Poggianti et al. 2016; Jaffé et al. 2018; Gullieuszik et al. 2020): weak RPS signature (JClass = 1, 2, 3; upper) and strong RPS signature (JClass = 4, 5; lower) in the jellyfish galaxies.
Paper: Enhanced Star Formation Activity of Extreme Jellyfish Galaxies in Massive Clusters and the Role of Ram Pressure Stripping
Authors: Jeong Hwan Lee, Myung Gyoon Lee, Jae Yeon Mun, Brian S. Cho, Jisu Kang
Figure caption: Distribution of the X-ray luminosity (L X) of the host clusters of jellyfish galaxies as a function of the cluster velocity dispersion (σ  v,cl). Green circles show the data of clusters observed by the GASP survey. Upside-down triangles show several well-known clusters: the Coma cluster (purple), A3627 (green), A1367 (yellow), and the Virgo cluster (magenta). The blue triangle shows the data of A1758N (EK19). Gray star symbols show cluster samples from the MACS and HFF surveys (Ebeling et al. 2007; Lotz et al. 2017; Richard et al. 2021). Red star symbols show the data of the five clusters (MACS J0916.1−0023, MACS J1752.0+4440, A2744, MACS J1258.0+4702, and MACS J1720.2+3536) in this study.
Paper: Enhanced Star Formation Activity of Extreme Jellyfish Galaxies in Massive Clusters and the Role of Ram Pressure Stripping
Authors: Jeong Hwan Lee, Myung Gyoon Lee, Jae Yeon Mun, Brian S. Cho, Jisu Kang
Figure caption: The SFR–M * diagrams of jellyfish galaxies from the GASP survey (upper left), the A901/2 supercluster (RO19; upper right), A1758N (EK19; lower left), and our GMOS/IFU study (lower right) compared with the SFMS at the median redshift of each sample. In the left panel, we mark jellyfish galaxies with strong RPS signatures as colored symbols and those with weak RPS signatures as gray symbols. Solid lines and shaded regions show the linear-fit lines of the SFMS and their uncertainty suggested by Speagle et al. (2014). Gray dashed lines denote the linear-fit line of the SFMS at z = 0.
Paper: Enhanced Star Formation Activity of Extreme Jellyfish Galaxies in Massive Clusters and the Role of Ram Pressure Stripping
Authors: Jeong Hwan Lee, Myung Gyoon Lee, Jae Yeon Mun, Brian S. Cho, Jisu Kang
Figure caption: Starburstiness (R SB) of jellyfish galaxies as a function of cluster velocity dispersion (σ  v,cl;  left), the ICM density (ρ ICM;  middle), and the degree of ram pressure (P ram;  right). Error bars in the left panel represent standard deviations of starburstiness of jellyfish galaxies in the same host clusters. We plot the data of jellyfish samples with strong RPS signatures as described in Figure 3. The Spearman’s rank correlation coefficients are shown at the top of each panel.
Paper: Enhanced Star Formation Activity of Extreme Jellyfish Galaxies in Massive Clusters and the Role of Ram Pressure Stripping
Authors: Jeong Hwan Lee, Myung Gyoon Lee, Jae Yeon Mun, Brian S. Cho, Jisu Kang
Figure caption: Total SFR (upper), tail SFR (middle), and the tail SFR fraction (f SFR;  lower) as a function of stellar mass (left) and cluster velocity dispersion (right). We plot our data (red star symbols) and 54 jellyfish galaxies observed by the GASP survey (green circles) for comparison.
Paper: First Experimental Confirmation of the CH3O + H2CO → CH3OH + HCO Reaction: Expanding the CH3OH Formation Mechanism in Interstellar Ices
Authors: Julia C. Santos, Ko-Ju Chuang, Thanja Lamberts, Gleb Fedoseev, Sergio Ioppolo, Harold Linnartz
Figure caption: CH3OH formation scheme involving H2CO and D2CO. The gray dashed line indicates the smaller efficiency of the deuterated radical-molecule reaction with relation to route (5).
Paper: First Experimental Confirmation of the CH3O + H2CO → CH3OH + HCO Reaction: Expanding the CH3OH Formation Mechanism in Interstellar Ices
Authors: Julia C. Santos, Ko-Ju Chuang, Thanja Lamberts, Gleb Fedoseev, Sergio Ioppolo, Harold Linnartz
Figure caption: Final IR spectra of the H2CO + H (red) and D2CO + H (black) codeposition experiments performed at 12 K. The spectra were obtained after 360 minutes of deposition and are artificially offset for clarity. Peak assignments are indicated with solid red (for H2CO + H) and black (for D2CO + H) lines, while the dashed gray line shows the absence of the CHD2OD ν ≈ 2420 cm−1 peak.
Paper: First Experimental Confirmation of the CH3O + H2CO → CH3OH + HCO Reaction: Expanding the CH3OH Formation Mechanism in Interstellar Ices
Authors: Julia C. Santos, Ko-Ju Chuang, Thanja Lamberts, Gleb Fedoseev, Sergio Ioppolo, Harold Linnartz
Figure caption: (a) Difference spectrum of the final spectra acquired after 360 minutes of H2CO + D codeposition minus that of the analogous D-atom beam deposition for the same time, both performed at 10 K. The dashed line indicates the absence of the CH2DOD feature at ν ∼ 2430 cm−1. (b) Infrared spectra obtained during the ramp-up after the H2CO + D 360 minutes codeposition. The gray, red, and blue spectra were measured at 10 K, 80–120 K, and 120–160 K, respectively.
Paper: First Experimental Confirmation of the CH3O + H2CO → CH3OH + HCO Reaction: Expanding the CH3OH Formation Mechanism in Interstellar Ices
Authors: Julia C. Santos, Ko-Ju Chuang, Thanja Lamberts, Gleb Fedoseev, Sergio Ioppolo, Harold Linnartz
Figure caption: Spectra of the TPD-QMS experiments obtained after codeposition of H2CO + H (upper) and D2CO + H (lower) at 12 K for 360 minutes. The m/z signals of 32 (red), 34 (blue), and 35 (green) correspond to, respectively, CH3OH, CHD2OH, and CHD2OD. No signal is detected for m/z = 35 at the desorption temperature of methanol (∼140 K).
Paper: First Experimental Confirmation of the CH3O + H2CO → CH3OH + HCO Reaction: Expanding the CH3OH Formation Mechanism in Interstellar Ices
Authors: Julia C. Santos, Ko-Ju Chuang, Thanja Lamberts, Gleb Fedoseev, Sergio Ioppolo, Harold Linnartz
Figure caption: Upper panel: yields of CH3OH and CHD2OH relative to the column density of CH3OH after 360 minutes of H2CO + H codeposition at 10, 12, 14, and 16 K, as derived from the RAIRS data. Lower panel: same as the upper panel, but for the TPD-QMS data. The reported values are normalized to the most abundant yield at 12 K.
Paper: Current-sheet Oscillations Caused by the Kelvin–Helmholtz Instability at the Loop Top of Solar Flares
Authors: Yulei Wang, Xin Cheng, Zining Ren, Mingde Ding
Figure caption: (a) The profiles of time-averaged local Alfvén speed at the CS outer boundary (the black curve) and the averaged propagation speeds of the CS oscillation (the blue curve). (b) The time-averaged density at the CS outer boundary. (c) The distributions of time-averaged magnetic strength at the CS outer boundary (the black curve) and the magnetic field strength evaluated by ﹩\langle {B}_{p}^{i}\rangle =\langle {V}_{p}^{i}\rangle \sqrt{\left\langle {\rho }_{\mathrm{Acs}}\right\rangle }﹩ (the blue curve). The CS outer boundaries are defined by x = ±0.05 and y > 0.75 (see Figure 2(d6)) and V Acs, ρ Acs, and B Acs are averaged values on both boundaries. ﹩\left\langle \cdot \right\rangle ﹩ denotes taking time-average in duration ﹩t\in \left[9,12\right]﹩.
Paper: Current-sheet Oscillations Caused by the Kelvin–Helmholtz Instability at the Loop Top of Solar Flares
Authors: Yulei Wang, Xin Cheng, Zining Ren, Mingde Ding
Figure caption: The CS structure at t = 9.1. (e) The temperature distribution of the CS at t = 9.1 (also see Figure 2(b1)). The blue, yellow, green, and brown slits are taken at y = 0.8, 1.1, 1.356, and 1.8 across the CS, respectively. (a1), (b1), (c1), and (d1) are, respectively, the profiles of ρ, T, J  z , and B  y  along the blue slit at y = 0.8. (a2)–(d2), (a3)–(d3), and (a4)–(d4) are the same as (a1)–(d1) but for different slits. The red dashed lines mark the positions with the maximum temperature gradient (﹩\left|\partial T/\partial x\right|﹩) on both sides of the CS, while the blue dashed lines denote the average positions of the red ones.