adsabs/AstroCLIMB huggingface dataset:
Paper: Gravitational Wave Sources in Our Galactic Backyard: Predictions for BHBH, BHNS, and NSNS Binaries Detectable with LISA
Authors: T. Wagg, F. S. Broekgaarden, S. E. de Mink, N. Frankel, L. A. C. van Son, S. Justham
Figure caption: Comparison of previous studies that are similar to this work. In the detection rate section, darker shades of blue indicate higher detection rates. In other sections, darker shades of green indicate more detailed models or more accurate choices. Entries in detection rates that list two values correspond to the different mission lengths (penultimate column). The works listed in the table are Nelemans et al. (2001), Belczynski et al. (2010), Liu & Zhang (2014), Lamberts et al. (2018), Sesana et al. (2020), Lau et al. (2020), Breivik et al. (2020), and Shao & Li (2021). </>
Paper: Gravitational Wave Sources in Our Galactic Backyard: Predictions for BHBH, BHNS, and NSNS Binaries Detectable with LISA
Authors: T. Wagg, F. S. Broekgaarden, S. E. de Mink, N. Frankel, L. A. C. van Son, S. Justham
Figure caption: As Figure 9, but instead varying the Wolf–Rayet wind efficiency (models S and T). The curve for f WR = 5 has much higher uncertainties because far fewer DCO systems form in this model (the inverse reasoning also explains the lower uncertainties for f WR = 0.1). </>
Paper: Gravitational Wave Sources in Our Galactic Backyard: Predictions for BHBH, BHNS, and NSNS Binaries Detectable with LISA
Authors: T. Wagg, F. S. Broekgaarden, S. E. de Mink, N. Frankel, L. A. C. van Son, S. Justham
Figure caption: As Figure 5, but for the chirp mass uncertainty. The shaded areas indicate regions with more than 10% and 100% uncertainty. </>
Paper: Gravitational Wave Sources in Our Galactic Backyard: Predictions for BHBH, BHNS, and NSNS Binaries Detectable with LISA
Authors: T. Wagg, F. S. Broekgaarden, S. E. de Mink, N. Frankel, L. A. C. van Son, S. Justham
Figure caption: As Figure 3(b), but for the Milky Way model used in Breivik et al. (2020). Dotted lines show the distribution from Figure 3(b) for comparison. </>
Paper: Gravitational Wave Sources in Our Galactic Backyard: Predictions for BHBH, BHNS, and NSNS Binaries Detectable with LISA
Authors: T. Wagg, F. S. Broekgaarden, S. E. de Mink, N. Frankel, L. A. C. van Son, S. Justham
Figure caption: As Figure 3(d), but for model Q. For comparison, we show the mean distribution for the fiducial model (model A) as dashed lines. </>
Paper: Gravitational Wave Sources in Our Galactic Backyard: Predictions for BHBH, BHNS, and NSNS Binaries Detectable with LISA
Authors: T. Wagg, F. S. Broekgaarden, S. E. de Mink, N. Frankel, L. A. C. van Son, S. Justham
Figure caption: As Figure 5, but for the angular resolution. </>
Paper: Gravitational Wave Sources in Our Galactic Backyard: Predictions for BHBH, BHNS, and NSNS Binaries Detectable with LISA
Authors: T. Wagg, F. S. Broekgaarden, S. E. de Mink, N. Frankel, L. A. C. van Son, S. Justham
Figure caption: As Figure 1 (right panel), but for the Milky Way model used in Breivik et al. (2020). </>
Paper: A Comprehensive Radiative Magnetohydrodynamics Simulation of Active Region Scale Flux Emergence from the Convection Zone to the Corona
Authors: Feng Chen, Matthias Rempel, Yuhong Fan
Figure caption: Left column: horizontally and temporally averaged temperature (a), density (c), and magnetic field strength (e) in the QS run. Dotted lines around the solid curves indicate the maximum and minimum values of the horizontally averaged temperature and density over the temporal evolution of about 11.5 hr. The dashed line at z = 5.28 Mm indicates the base of the corona. Right column: probability density functions (PDFs) of the temperature, density, and magnetic field strength in a snapshot at t QS = 5.7 hr. The PDFs are evaluated and normalized to unity at each height.
Paper: A Comprehensive Radiative Magnetohydrodynamics Simulation of Active Region Scale Flux Emergence from the Convection Zone to the Corona
Authors: Feng Chen, Matthias Rempel, Yuhong Fan
Figure caption: Examples of campfire-like small-scale transient brightenings. Panel (a): synthetic AIA 171 image from the top view of the whole horizontal domain. Red boxes (10 Mm wide each) mark four examples shown in a detailed view in panels (b)–(e), respectively. These images are displayed with the same color scale (0–1000 DN pixel−1 s−1) as in Figure 3.
Paper: A Comprehensive Radiative Magnetohydrodynamics Simulation of Active Region Scale Flux Emergence from the Convection Zone to the Corona
Authors: Feng Chen, Matthias Rempel, Yuhong Fan
Figure caption: Coronal dimming created in the quiet Sun by an emerging active region. Panel (a): B  z  at the photosphere, before the active region emerges. Panel (b): B  z  as in panel (a), but when a flux concentration (at (x,y) = (120,50)) starts to form. Panels (c) and (d): synthetic AIA 193 channel images from the top view. The time stamps are the same as in panels (a) and (b), respectively. The dimming region is visible in the lower half of the field of view. Panels (e) and (f): synthetic AIA 193 channel images from a side view along the y-axis. The time stamps are the same as in panels (a) and (b), respectively.
Paper: A Comprehensive Radiative Magnetohydrodynamics Simulation of Active Region Scale Flux Emergence from the Convection Zone to the Corona
Authors: Feng Chen, Matthias Rempel, Yuhong Fan
Figure caption: Evolution of coronal thermodynamics in the dimming region over an emerging active region. Panels (a) and (b): emission measure (EM) weighted temperature from a side view along the y-axis, as defined in Equation (16). The time stamps are the same as in Figure 15. Panels (c) and (d): mean density derived from emission measures, as in Equation (17). Panel (e): change in the mean temperature and density of the corona above the emerging active region (averaged within the boxes marked in panels (a)–(d)). The solid and dotted lines show the mean temperature and density, respectively. Panel (f): change in the mean emission measure in the corona above the emerging active region (averaged within the box marked in panels (a)–(d)). The blue line shows the mean emission measure in ﹩\mathrm{log}T=[6.0,6.3)﹩, and the red line is for ﹩\mathrm{log}T=[6.3,6.5)﹩. The black dotted line shows the unsigned magnetic flux in the photosphere.
Paper: A Comprehensive Radiative Magnetohydrodynamics Simulation of Active Region Scale Flux Emergence from the Convection Zone to the Corona
Authors: Feng Chen, Matthias Rempel, Yuhong Fan
Figure caption: Horizontally averaged r  f  as a function of height. The black line shows the simple arithmetic mean at each height. The blue line plots the current-weighted mean. The red line depicts the most probable values of r  f  (the same as the white line in Figure 13(a)).
Paper: A Comprehensive Radiative Magnetohydrodynamics Simulation of Active Region Scale Flux Emergence from the Convection Zone to the Corona
Authors: Feng Chen, Matthias Rempel, Yuhong Fan
Figure caption: T-D diagrams of emission measures in four temperature bins showing the onset, propagation, and decay of the jet seen in Figure 18 and associated animation. The diagram is constructed for the duration of the jet (about 10 minutes) and along the dotted line in Figure 18. The EM in each panel is shown relative to the mean value.
Paper: Stratified Distribution of Organic Molecules at the Planet-formation Scale in the HH 212 Disk Atmosphere
Authors: Chin-Fei Lee, Claudio Codella, Cecilia Ceccarelli, Ana López-Sepulcre
Figure caption: Total line intensity maps of NH2CHO, HNCO, t-HCOOH, H2CO, D2CO, H2 13CO, CH3OH, and CH3CHO (red contours) on top of the 1.33 mm continuum map (gray image with black contours) toward the HH 212 disk. The maps are rotated clockwise by ∼23° so that the disk is aligned horizontally for easy view. For the continuum, the contours start from 10 K with a step of 15 K. The line intensity maps are integrated over velocity within ∼4.0 km s−1 of the systemic velocity (which is ∼ 1.7 ± 0.1 km s−1 LSR Lee et al. 2014). As described in the text, we divided the lines into two ranges of upper-level energies: E  u  < 120 K and E  u  > 120 K, and then stacked them for each species for higher sensitivity. The asterisk marks the possible position of the central protostar. The vertical cyan lines mark the centrifugal barrier. The contours start at 3σ with a step of 2σ, where σ are (a) 1.5, (b) 0.8, (d) 2.1, (e) 1.3, (f) 4.0, (g) 2.4, (h) 2.6, (i) 3.4, (j) 1.6, (k) 1.8, and (l) 1.4 mJy beam−1. The blue circle in (j) marks the emission peak used to derive the physical properties of CH3OH.
Paper: Stratified Distribution of Organic Molecules at the Planet-formation Scale in the HH 212 Disk Atmosphere
Authors: Chin-Fei Lee, Claudio Codella, Cecilia Ceccarelli, Ana López-Sepulcre
Figure caption: Physical properties of CH3OH toward the disk atmosphere. (a) and (b) show the results of the non-LTE LVG analysis using the lines with E  u  < 200 K with the GRELVG code (Ceccarelli et al. 2003), while (c) shows the result of the rotation diagram using the lines with E  u  > 200 K. The line intensity is extracted from an emission peak in the lower disk atmosphere, as marked by a blue circle in Figure 1(j). (a) Density–Temperature χ 2 contour plot. The contour represents a 1σ confidence level, assuming the best-fit values of N(A-CH3OH) and N(E-CH3OH). The best-fit solution is marked by the cross. (b) The ratio between the observed line intensities (circles for A-type and squares for E-type) with those of the best fit as a function of E  u . (c) Rotation diagram of CH3OH with the same symbols. The solid line is a linear fit to the data. The optically thick lines are marked with open squares and circles and excluded from the fitting.
Paper: Stratified Distribution of Organic Molecules at the Planet-formation Scale in the HH 212 Disk Atmosphere
Authors: Chin-Fei Lee, Claudio Codella, Cecilia Ceccarelli, Ana López-Sepulcre
Figure caption: (a) Continuum map (black contours and gray image, same as Figure 1(c)), continuum optical depth (blue contours, with contour levels 1, 3, and 5) at λ ∼ 1.33 mm (or 226 GHz), NH2CHO (red contours, same as Figure 1(a)) and CH3OH (cyan contours, same as Figure 1(j)) total line intensity maps. (b) Stratification of various molecules in the disk atmosphere plotted on the temperature structure of the dusty disk adopted from Lee et al. (2021b). The crosses mark the outer radius and vertical height measured from the observations. The upper limit of the outer radius of HDO estimated at 60 au resolution by Codella et al. (2018) is also marked.
Paper: Stratified Distribution of Organic Molecules at the Planet-formation Scale in the HH 212 Disk Atmosphere
Authors: Chin-Fei Lee, Claudio Codella, Cecilia Ceccarelli, Ana López-Sepulcre
Figure caption: Rotation diagrams for molecular lines of NH2CHO, HNCO, and CH3CHO. The diagrams are derived from the line intensities in the lower disk atmosphere listed in Table 1. The error bars show the uncertainty in our measurements, which are assumed to be 40% of the data values. The solid line is a linear fit to the data. The blended lines of NH2CHO are excluded from the diagram. The optically thick line of HNCO is marked with an open square and excluded from the fitting. For CH3CHO, the temperature is fixed at 100 K.
Paper: Stratified Distribution of Organic Molecules at the Planet-formation Scale in the HH 212 Disk Atmosphere
Authors: Chin-Fei Lee, Claudio Codella, Cecilia Ceccarelli, Ana López-Sepulcre
Figure caption: Position–velocity diagrams of various molecular lines cut across the upper and lower atmospheres of the disk. The contours start from 3σ with a step of 2σ, where σ are 0.36, 0.51, 0.70, 0.51, 0.43, 0.70, and 0.22 mJy beam−1 for NH2CHO, HNCO, t-HCOOH, H2CO, CH3OH, D2CO, and CH3CHO, respectively. The vertical lines mark the systemic velocity. The horizontal lines mark the center of the atmosphere. We also plot the Keplerian rotation curves (blue curves) due to a central mass of 0.25 M ⊙ (Lee et al. 2017c). The magenta lines roughly mark the linear velocity gradients of the PV structures in the upper atmosphere.
Paper: The Origin of the Vanishing Soft X-Ray Excess in the Changing-look Active Galactic Nucleus Mrk 590
Authors: Ritesh Ghosh, Sibasish Laha, Kunal Deshmukh, Varun Bhalerao, Gulab C. Dewangan, Ritaban Chatterjee
Figure caption: The X-ray and UV parameters of the central engine of the AGN Mrk 590, as observed by XMM-Newton, Suzaku, NuSTAR, and Swift (see Table 5 for details). The start date of 2002 January 1 corresponds to the first XMM-Newton observation (obs1). The X-axis is in units of days elapsed from the start date. From top to bottom: (1) the soft excess flux in the 0.3–2 keV band (in units of 10−13 erg cm−2 s−1), (2) the power-law flux in the 2–10  keV band (in units of 10−13 erg cm−2 s−1), (3) the UV (UVW1) monochromatic flux density at 2500 Å (in units of 10−15 erg cm−2 s−1), (4) the Fe emission-line flux (in units of 10−13 erg cm2 s−1 Å−1), (5) the α OX, and (6) the Eddington ratio (λ Edd). The vertical line represents the epoch up to when soft excess is present.
Paper: The Origin of the Vanishing Soft X-Ray Excess in the Changing-look Active Galactic Nucleus Mrk 590
Authors: Ritesh Ghosh, Sibasish Laha, Kunal Deshmukh, Varun Bhalerao, Gulab C. Dewangan, Ritaban Chatterjee
Figure caption: The correlation plot between the 0.3 and 2.0 keV soft excess emission flux and the accretion rate, λ Edd, for all six observations where simultaneous optical–UV data are available. Hence, the two Suzaku observations are not considered. The figure shows no significant correlation between the two fluxes (R  s  = 0.086).
Paper: The Origin of the Vanishing Soft X-Ray Excess in the Changing-look Active Galactic Nucleus Mrk 590
Authors: Ritesh Ghosh, Sibasish Laha, Kunal Deshmukh, Varun Bhalerao, Gulab C. Dewangan, Ritaban Chatterjee
Figure caption: Top left: the relationship between the 2500 Å luminosity and α OX of the CLAGN Mrk 590 showing lack of anticorrelation. Top right: the relationship between the logarithm of the luminosity at 2 keV and the UV monochromatic luminosity at 2500 Å of the CLAGN Mrk 590. Bottom left: the relationship between the logarithm of the Eddington ratio and the power-law slope of the CLAGN Mrk 590. Bottom right: the correlation plot between the UV monochromatic flux at 2500 Å and the 2–10  keV power-law flux. We calculated the Spearman’s correlation coefficient (R  s  = 0.714) and did not find any significant correlation between the two fluxes. The two Suzaku observations are not considered, as simultaneous optical–UV data are not available.
Paper: The Origin of the Vanishing Soft X-Ray Excess in the Changing-look Active Galactic Nucleus Mrk 590
Authors: Ritesh Ghosh, Sibasish Laha, Kunal Deshmukh, Varun Bhalerao, Gulab C. Dewangan, Ritaban Chatterjee
Figure caption: The best-fit UV/X-ray models for 2002 January (black circle), 2004 July (red diamond), 2016 February (green square), 2018 October (blue star), 2020 January (cyan triangle), and 2021 (magenta cross) derived using two XMM-Newton and four simultaneous Swift plus NuSTAR observations. The ionized reflection model describing the soft excess and power-law emission and the optical–UV emission described by the diskbb are shown for each epoch with different markers and colors. The MyTorusL (dotted lines) and MyTorusS (dashed lines) components for each epoch are shown with the same colors. The 2016 (green square) and 2020 (cyan triangle) observations represent the lowest and highest flux state of the source, respectively. The two Suzaku observations are not considered owing to the absence of simultaneous optical–UV data.
Paper: The Origin of the Vanishing Soft X-Ray Excess in the Changing-look Active Galactic Nucleus Mrk 590
Authors: Ritesh Ghosh, Sibasish Laha, Kunal Deshmukh, Varun Bhalerao, Gulab C. Dewangan, Ritaban Chatterjee
Figure caption: The correlation plot between the 0.3 and 2.0 keV soft excess emission flux and the UV monochromatic (2500 Å) flux. We do not see any significant correlation (R  s  = −0.314). The two Suzaku observations are not considered, as simultaneous optical–UV data are not available.
Paper: The Origin of the Vanishing Soft X-Ray Excess in the Changing-look Active Galactic Nucleus Mrk 590
Authors: Ritesh Ghosh, Sibasish Laha, Kunal Deshmukh, Varun Bhalerao, Gulab C. Dewangan, Ritaban Chatterjee
Figure caption: The correlation plot between the 0.3 and 2.0  keV soft excess emission flux and the 2–10  keV power-law flux. We did not find any significant correlation between the two fluxes (R  s  = −0.314).
Paper: The Origin of the Vanishing Soft X-Ray Excess in the Changing-look Active Galactic Nucleus Mrk 590
Authors: Ritesh Ghosh, Sibasish Laha, Kunal Deshmukh, Varun Bhalerao, Gulab C. Dewangan, Ritaban Chatterjee
Figure caption: The 0.001–50.0 keV simultaneous Swift and NuSTAR spectra of Mrk 590 fitted with an absorbed optxagnf and MyTorus model. The broadband data, the residuals, and the theoretical model are shown for obs7 and obs8. We see that the set of models fails to describe the high-energy cutoff of primary continuum observed above 20 keV. We fitted each data set separately. The X-axis represents observed-frame energy.
Paper: The Origin of the Vanishing Soft X-Ray Excess in the Changing-look Active Galactic Nucleus Mrk 590
Authors: Ritesh Ghosh, Sibasish Laha, Kunal Deshmukh, Varun Bhalerao, Gulab C. Dewangan, Ritaban Chatterjee
Figure caption: The confidence interval plot of the high-energy cutoff parameter E cut of four observations, obs4, obs6, obs7, and obs8. The top panel shows the confidence contour plot of obs4 and obs6, among others that could not be constrained owing to low-quality data above 20 keV. We found similar results for obs3 and obs5. The bottom panel shows the same contour plot for obs7 and obs8, which are well constrained.
Paper: Relationship between Successive Flares in the Same Active Region and SHARP Parameters
Authors: Hao Ran, Ying D. Liu, Yang Guo, Rui Wang
Figure caption: The eight parameters in the whole AR and in the PIL area for AR 11283. Two adjacent panels, such as panel (a) and (b), belong to a group of the same SHARP. In the same group, the left panel is the SHARP in the whole AR, and the right one is the SHARP in the PIL area. Counting from left to right and up to down, the eight groups are “TOTPOT,” “MEANPOT,” “USFLUX,” “MEANGAM,” “MEANGBH,” “MEANJZH,” “MEANSHR,” and “MEANALP.” Each panel is labeled with a letter from (a) to (p). The SHARP parameters are normalized. The corresponding correlation coefficient (CC) is at the top of each panel. The maximum value of each SHARP parameter is also at the top. Similar format to Figure 2.
Paper: Ultraviolet Spectroscopy and TARDIS Models of the Broad-lined Type Ic Supernova 2014ad
Authors: Lindsey A. Kwok, Marc Williamson, Saurabh W. Jha, Maryam Modjaz, Yssavo Camacho-Neves, Ryan J. Foley, Peter Garnavich, Keiichi Maeda, Dan Milisavljevic, Viraj Pandya, Mi Dai, Curtis McCully, Tyler Pritchard, Jaladh Singhal
Figure caption: Optical spectral time series of SN 2014ad. We present 22 epochs from SALT (black), two epochs from HST (yellow; 2014 March 19 and 2014 March 25), two epochs from LBT (yellow; 2014 June 4, 2015 January 20), and two epochs from Magellan (yellow; 2014 August 2 and 2015 January 16). We display published spectra from (Sahu et al. 2018, blue) and (Stevance et al. 2017, red) as well as two unpublished epochs (gray) from PESSTO (Smartt et al. 2015) via WISeREP (Yaron & Gal-Yam 2012). The wavelength axis is redshift-corrected to the host-galaxy rest frame. The fluxes have been corrected for total reddening and are scaled and vertically shifted for clarity. Cosmic rays, narrow host-galaxy lines, and telluric absorption have been removed in all spectra. The phase is given in rest-frame days relative to B maximum light (MJD 56735.11; Sahu et al. 2018).
Paper: Ultraviolet Spectroscopy and TARDIS Models of the Broad-lined Type Ic Supernova 2014ad
Authors: Lindsey A. Kwok, Marc Williamson, Saurabh W. Jha, Maryam Modjaz, Yssavo Camacho-Neves, Ryan J. Foley, Peter Garnavich, Keiichi Maeda, Dan Milisavljevic, Viraj Pandya, Mi Dai, Curtis McCully, Tyler Pritchard, Jaladh Singhal
Figure caption: Complete ultraviolet (UV) to near-infrared (NIR) spectra of SN 2014ad at two epochs near maximum light. We present HST/STIS spectroscopy of SN 2014ad covering the UV and optical wavelength ranges. The 2014 March 19 HST spectrum corresponds to a phase of +1 day (blue) and the 2014 March 25 HST spectrum corresponds to a phase of +7 days (red) past B maximum light. NIR spectra of SN 2014ad from Shahbandeh et al. (2022) at closely matching epochs of +0 day (black) and +7 days (gray) are plotted alongside the UV+Optical spectra to show the complete composite spectrum. The spectra have been plotted on a log–log scale to emphasize the UV and NIR data, while the inset shows the data on a log-linear scale.
Paper: Relationship between Successive Flares in the Same Active Region and SHARP Parameters
Authors: Hao Ran, Ying D. Liu, Yang Guo, Rui Wang
Figure caption: Scatter diagrams for the ranking of different SHARP parameters calculated from NGBoost. The left panel shows the ranking for the parameter “location” in the possibility distribution, and the right one shows the ranking for the parameter “scale.” Inside the blue ellipse are the parameters of the greatest importance.
Paper: Ultraviolet Spectroscopy and TARDIS Models of the Broad-lined Type Ic Supernova 2014ad
Authors: Lindsey A. Kwok, Marc Williamson, Saurabh W. Jha, Maryam Modjaz, Yssavo Camacho-Neves, Ryan J. Foley, Peter Garnavich, Keiichi Maeda, Dan Milisavljevic, Viraj Pandya, Mi Dai, Curtis McCully, Tyler Pritchard, Jaladh Singhal
Figure caption: Finding chart for the 2014 August 2 spectrum of SN 2014ad from Magellan+IMACS. SN 2014ad is located in PGC 37625 (Markarian 1309) and was difficult to observe due to the nearby V = 7.4 mag star.
Paper: Relationship between Successive Flares in the Same Active Region and SHARP Parameters
Authors: Hao Ran, Ying D. Liu, Yang Guo, Rui Wang
Figure caption: The importance feature of the SHARP parameters in AR 12673. The left panel refers to the importance feature distribution of “location,” and the right panel refers to the importance feature distribution of “scale.”
Paper: Relationship between Successive Flares in the Same Active Region and SHARP Parameters
Authors: Hao Ran, Ying D. Liu, Yang Guo, Rui Wang
Figure caption: The original flare envelope and the corresponding “flare envelope” calculated from NGBoost for the six selected ARs. The green curves are the original flare envelopes, and the blue curves are from NGBoost.
Paper: Relationship between Successive Flares in the Same Active Region and SHARP Parameters
Authors: Hao Ran, Ying D. Liu, Yang Guo, Rui Wang
Figure caption: Comparison between the original flare envelope and the “flare envelope” curve calculated from NGBoost with the selected eight SHARP parameters only.
Paper: MHD Simulations of Dense Core Collision
Authors: Shinichi W. Kinoshita, Fumitaka Nakamura
Figure caption: Column density, magnetic field, and velocity distributions of the model b0-M1-By10. First row: column density maps. The black vectors indicate the mass-weighted velocity field. Velocity arrows scale linearly with respect to the reference velocity shown in the bottom right of the panel and corresponding to 0.3 km · s−1. Second row: mass-weighted magnetic field strength of cloud material are shown directly below their corresponding column-density maps. White pseudovectors indicate the normalized plane-of-sky magnetic polarization field,  p .
Paper: MHD Simulations of Dense Core Collision
Authors: Shinichi W. Kinoshita, Fumitaka Nakamura
Figure caption: Temporal evolution of mass accretion rate of sink particles for head-on (b = 0) cases. Left panel: ﹩{ \mathcal M }=1﹩ models. Right panel: ﹩{ \mathcal M }=3﹩ models.
Paper: MHD Simulations of Dense Core Collision
Authors: Shinichi W. Kinoshita, Fumitaka Nakamura
Figure caption: Initial conditions with the mass surface density shown. White arrows indicate the direction of each core’s motion. Left panel: Head-on collision cases (b = 0). Right panel: off-center collision cases (b=r c).