adsabs/AstroCLIMB huggingface dataset:
Paper: Total Solar Irradiance during the Last Five Centuries
Authors: Valentina Penza, Francesco Berrilli, Luca Bertello, Matteo Cantoresi, Serena Criscuoli, Piermarco Giobbi
Figure caption: Same as in Figure 5, but for sunspot data. Here, the light green region shows the 20σ confidence interval of the mean annual value.
Paper: Potential Signature of Population III Pair-instability Supernova Ejecta in the BLR Gas of the Most Distant Quasar at z = 7.54 
Authors: Yuzuru Yoshii, Hiroaki Sameshima, Takuji Tsujimoto, Toshikazu Shigeyama, Timothy C. Beers, Bruce A. Peterson
Figure caption: [Mg/Fe] (upper panel) and [Fe/H] (lower panel) as a function of the age of the Universe, plotted as filled magenta circles for the results of ULAS J1342 and z < 3 samples from Sameshima et al. (2017, 2020). The green and blue curves are the standard chemical evolution models for the core region of an elliptical galaxy for two cases with different delay-time distributions of SNe Ia. The red curve is the variant model in which SN Ia ejecta predominates in the early Galaxy.
Paper: Potential Signature of Population III Pair-instability Supernova Ejecta in the BLR Gas of the Most Distant Quasar at z = 7.54 
Authors: Yuzuru Yoshii, Hiroaki Sameshima, Takuji Tsujimoto, Toshikazu Shigeyama, Timothy C. Beers, Bruce A. Peterson
Figure caption: [Mg/Fe] (upper panel) and [Fe/H] (lower panel) as a function of the age of the Universe. Same as Figure 3, but the alternative chemical evolution models for the core region of an elliptical galaxy, which is thought to host ULAS J1342, are shown by thick curves, in addition to the standard models. The alternative models are calculated by assuming that a fraction of the BLR gas with [Fe/H] = +1.3 and [Mg/Fe] = −1 is initially mixed with the metal-free gas in the core region of the elliptical galaxy, and that the chemical evolution in the core region starts with [Fe/H] = −4 and [Mg/Fe] = −1 at z = 8 (see the text in Section 3). The color-coded rectangular regions indicate the values of [Mg/Fe] and [Fe/H] as a function of progenitor mass of Pop III PISN. The width of these regions corresponds to the transition period of cosmological reionization.
Paper: Potential Signature of Population III Pair-instability Supernova Ejecta in the BLR Gas of the Most Distant Quasar at z = 7.54 
Authors: Yuzuru Yoshii, Hiroaki Sameshima, Takuji Tsujimoto, Toshikazu Shigeyama, Timothy C. Beers, Bruce A. Peterson
Figure caption: Comparison of the form of L *(z) in the Global fit A model with observed data. The gray dots indicate the SDSS quasars analyzed by Sameshima et al. (2017), together with the mean and standard deviation for each redshift bin. The circles indicate the z ∼ 2.7 quasars analyzed by Sameshima et al. (2020), and the star indicates ULAS J1342. The solid blue line is L *(z) of the Global fit A model in Shen et al. (2020), scaled to fit the mean L 3000 of the SDSS quasars, and the dashed blue line is its extrapolation to z > 7.
Paper: Lorentz Invariance Violation Test from Time Delays Measured with Gravitationally Lensed GRB Candidates 950830 and 200716C
Authors: Lin Lan, Aleksandra Piórkowska-Kurpas, Xudong Wen, Marek Biesiada, Kai Liao, He Gao, Zhengxiang Li
Figure caption: Energy dependence of the observed gravitational lensing time delays ΔLIV(Δt PM) (relative to the softest energy band), and the best-fit theoretical curves (red solid line)—the linear (n = 1) LIV model.
Paper: Lorentz Invariance Violation Test from Time Delays Measured with Gravitationally Lensed GRB Candidates 950830 and 200716C
Authors: Lin Lan, Aleksandra Piórkowska-Kurpas, Xudong Wen, Marek Biesiada, Kai Liao, He Gao, Zhengxiang Li
Figure caption: The quantity J  n (z  l , z  s ) as a function of source redshift z  s  in different configurations of lens redshift z  l  for the linear (n = 1) LIV model (red line style) and the quadratic (n = 2) LIV model (blue line style).
Paper: Potential Signature of Population III Pair-instability Supernova Ejecta in the BLR Gas of the Most Distant Quasar at z = 7.54 
Authors: Yuzuru Yoshii, Hiroaki Sameshima, Takuji Tsujimoto, Toshikazu Shigeyama, Timothy C. Beers, Bruce A. Peterson
Figure caption: Parameters obtained by fitting the EWs of the SDSS quasars measured by Sameshima et al. (2017) with Equation (4) as a function of redshift. The Mg II results are shown in green, and the Fe II results are shown in purple. Dashed lines represent the results of the fitting when all SDSS samples are used without binning by redshift.
Paper: Multispacecraft Analysis of the Properties of Magnetohydrodynamic Fluctuations in Sub-Alfvénic Solar Wind Turbulence at 1 au
Authors: S. Q. Zhao, Huirong Yan, Terry Z. Liu, Mingzhe Liu, Huizi Wang
Figure caption: An overview of solar wind fluctuations from MMS1 and OMNI. (a)–(g) Event 1: during 23:00–02:00 UT on 2017 November 23–24. (h)–(n) Event 2: during 21:00–23:00 UT on 2017 November 26. (o)–(u) Event 3: during 20:15–22:15 UT on 2017 November 14. The panels from top to bottom show the magnetic field magnitude ∣B∣, magnetic field components in GSE, relative amplitudes of the magnetic field δ B rms/∣B 0∣, comparisons of fluctuating magnetic field and background magnetic field in GSE, the spectrogram of ion differential energy fluxes (in units of keV cm−2 s−1 sr−1 keV−1), proton plasma β  p , and wave propagation angles with respect to the background magnetic field.
Paper: Multispacecraft Analysis of the Properties of Magnetohydrodynamic Fluctuations in Sub-Alfvénic Solar Wind Turbulence at 1 au
Authors: S. Q. Zhao, Huirong Yan, Terry Z. Liu, Mingzhe Liu, Huizi Wang
Figure caption: A schematic of MMS locations in GSE coordinates. Blue and red solid curves represent the empirical models of the terrestrial bow shock (Peredo et al. 1995) and magnetopause (Roelof & Sibeck 1993), respectively. The black, red, and blue arrows represent the directions of the background magnetic field for Event 1 ([17, 18, 6] R  E ), Event 2 ﹩([17,17,6]\,{R}_{E})﹩, and Event 3 ﹩([17,17,6]\,{R}_{E})﹩, respectively.
Paper: Comprehensive Analysis of the Neutrino Process in Core-collapsing Supernovae
Authors: Heamin Ko, Dukjae Jang, Myung-Ki Cheoun, Motohiko Kusakabe, Hirokazu Sasaki, Xingqun Yao, Toshitaka Kajino, Takehito Hayakawa, Masaomi Ono, Toshihiko Kawano, Grant J. Mathews
Figure caption: The same as Figure 20, but for 180Ta.
Paper: Comprehensive Analysis of the Neutrino Process in Core-collapsing Supernovae
Authors: Heamin Ko, Dukjae Jang, Myung-Ki Cheoun, Motohiko Kusakabe, Hirokazu Sasaki, Xingqun Yao, Toshitaka Kajino, Takehito Hayakawa, Masaomi Ono, Toshihiko Kawano, Grant J. Mathews
Figure caption: The same as Figure 20, but for 92Nb.
Paper: Comprehensive Analysis of the Neutrino Process in Core-collapsing Supernovae
Authors: Heamin Ko, Dukjae Jang, Myung-Ki Cheoun, Motohiko Kusakabe, Hirokazu Sasaki, Xingqun Yao, Toshitaka Kajino, Takehito Hayakawa, Masaomi Ono, Toshihiko Kawano, Grant J. Mathews
Figure caption: The same as Figure 20, but for 138La.
Paper: Comprehensive Analysis of the Neutrino Process in Core-collapsing Supernovae
Authors: Heamin Ko, Dukjae Jang, Myung-Ki Cheoun, Motohiko Kusakabe, Hirokazu Sasaki, Xingqun Yao, Toshitaka Kajino, Takehito Hayakawa, Masaomi Ono, Toshihiko Kawano, Grant J. Mathews
Figure caption: The same as Figure 20, but for 11C.
Paper: Comprehensive Analysis of the Neutrino Process in Core-collapsing Supernovae
Authors: Heamin Ko, Dukjae Jang, Myung-Ki Cheoun, Motohiko Kusakabe, Hirokazu Sasaki, Xingqun Yao, Toshitaka Kajino, Takehito Hayakawa, Masaomi Ono, Toshihiko Kawano, Grant J. Mathews
Figure caption: The same as Figure 20, but for 98Tc.
Paper: Comprehensive Analysis of the Neutrino Process in Core-collapsing Supernovae
Authors: Heamin Ko, Dukjae Jang, Myung-Ki Cheoun, Motohiko Kusakabe, Hirokazu Sasaki, Xingqun Yao, Toshitaka Kajino, Takehito Hayakawa, Masaomi Ono, Toshihiko Kawano, Grant J. Mathews
Figure caption: The same as Figure 20, but for 7Be.
Paper: Comprehensive Analysis of the Neutrino Process in Core-collapsing Supernovae
Authors: Heamin Ko, Dukjae Jang, Myung-Ki Cheoun, Motohiko Kusakabe, Hirokazu Sasaki, Xingqun Yao, Toshitaka Kajino, Takehito Hayakawa, Masaomi Ono, Toshihiko Kawano, Grant J. Mathews
Figure caption: The same as Figure 20, but for 11B.
Paper: Stellar Energetic Particle Transport in the Turbulent and CME-disrupted Stellar Wind of AU Microscopii
Authors: Federico Fraschetti, Julián D. Alvarado-Gómez, Jeremy J. Drake, Ofer Cohen, Cecilia Garraffo
Figure caption: Top: in the 90 minutes post-CME case based on the Klein et al. (2021b) magnetogram as in Figure 8, the EP hitting points on the R  b  sphere are seen from the side of the two CME expanding lobes. The strength of the unperturbed wind magnetic field B 0 color codes the R  b  sphere. The two magenta circles represent the orbits of planet b (solid) and c (dotted). The purple lines indicate selected closed magnetic field lines. Open magnetic field lines are in green or black if one end is attached to the star surface or if none of the ends is tracked, respectively. Middle: same as the top left but from the back side. Bottom: snapshot in a 180 R ⋆ field of view of the bi-lobed plasma density isosurface (n(x, t)/n  SS (x) = 10.0) of the propagating CME within the wind reconstructed from the ZDI maps of Klein et al. (2021b) at 90 minutes past the CME initiation. The spherical dots at R  b /2, R  b , and R  c  mark the EP hitting points and are color coded by the B-field strength. The two cyan circles represent the orbits of planet b (solid) and c (dotted). Open magnetic field lines are in black.
Paper: Origin of Nitrogen Isotopic Variations in the Rocky Bodies of the Solar System
Authors: Damanveer S. Grewal
Figure caption: Isotopic compositions of the rocky bodies from NC and CC reservoirs plotted in δ 15N–ε 54Cr, δ 15N–ε 50Ti, and δ 15N–Δ95Mo space. Even though δ 15N values of NC meteorites (red) are generally lower than CC meteorites (blue), unlike ε 54Cr, ε 50Ti, and Δ95Mo values, there is an overlap between the δ 15N values of NC and CC meteorites. δ and ε are the measure of isotopic ratios in parts per 1000 and 10,000, respectively. Δ95Mo (=[ε 95Mo—0.596 × ε 94Mo] × 100) is the vertical deviation from the s-process mixing line (Budde et al. 2019). Error bars for ε 54Cr, ε 50Ti, and Δ95Mo values are 2σ of the mean of the measurements, whereas for δ 15N values error bars are 1σ of the mean of the measurements. If absent, error bars are smaller than the symbol size. δ 15N values of meteorites are tabulated in Table 1. Data for the ε 54Cr, ε 50Ti, and Δ95Mo values is compiled from Spitzer et al. (2020).
Paper: Origin of Nitrogen Isotopic Variations in the Rocky Bodies of the Solar System
Authors: Damanveer S. Grewal
Figure caption: Nitrogen isotopic compositions of meteorites as a function of their accretion ages. δ 15N values of planetesimals (except IIE irons) accreting within ∼3 Ma after CAIs lie in a similar range followed by an increase for later accreting CM, CI, Tagish Lake, and CR chondrites. Note that the symbols of groups IID, IIF, IIIF, and IVB of CC iron meteorites are overprinted due to an overlap in their δ 15N values and accretion ages.
Paper: Stellar Energetic Particle Transport in the Turbulent and CME-disrupted Stellar Wind of AU Microscopii
Authors: Federico Fraschetti, Julián D. Alvarado-Gómez, Jeremy J. Drake, Ofer Cohen, Cecilia Garraffo
Figure caption: Left: fraction of 1 GeV EPs reaching a given sphere at radius R to the total number of injected EPs, N inj as a function of σ 2 in the stellar wind reconstructed from the ZDI maps of Klein et al. (2021b). The quiescent case (labeled as “Q”) is compared with the 90 minutes post-CME case (“CME”). The red filled circles refer to the flare case (R  s  = 1.2 R ⋆; Figure 7) corresponding, from lowest to highest N(R)/N inj to R = 0.15R  b , R  b /4, R  b /2, and R  b . Right: same as the left panel but for the stellar wind reconstructed from the ZDI maps of Kochukhov & Reiners (2020), case 1 from (Alvarado-Gómez et al. 2022), in the 90 minutes post-CME case.
Paper: Origin of Nitrogen Isotopic Variations in the Rocky Bodies of the Solar System
Authors: Damanveer S. Grewal
Figure caption: Nitrogen isotopic compositions of bulk chondrites and IOM residues compared with the effective temperatures (T eff) of chondritic samples inferred from organic thermometry. Nitrogen contents as well as δ 15N values decrease sharply with an increasing degree of thermal metamorphism in planetesimals. The variation of N contents and δ 15N values at a given T eff is likely a result of varying aqueous alteration. T eff data is compiled from Cody et al. (2008). Refer to Table 2 for data compilation.
Paper: Stellar Energetic Particle Transport in the Turbulent and CME-disrupted Stellar Wind of AU Microscopii
Authors: Federico Fraschetti, Julián D. Alvarado-Gómez, Jeremy J. Drake, Ofer Cohen, Cecilia Garraffo
Figure caption: Comparison of the 1 GeV proton scattering mean free path as a function of radial distance from the host star, both in units of R ⋆, for quiescent AU Mic (magnetogram from Klein et al. 2021b) and TRAPPIST-1 (Fraschetti et al. 2019), for σ 2 = 1 (left y-axis) and for σ 2 = 0.01 (right y-axis) at four locations for TRAPPIST-1 and five for AU Mic. Two values of R  s  (“Inj”) are seen, the half and full radius of AU Mic b’s orbit and semimajor axis of TRAPPIST-1e and AU Mic c. The value of λ ∥ is calculated from Equation (2) by using a typical magnetic field strength at the boundary between the CS stripe and the open field lines region, as inferred from the maps in Figure 3 and in Figure 10 of Fraschetti et al. (2019). The red/blue (AU Mic/TRAPPIST-1) shaded areas indicate the HZs from the inner boundary (0.22 au for AU Mic and 0.017 au for TRAPPIST-1) to the outer boundary (0.035 au for TRAPPIST-1).
Paper: Stellar Energetic Particle Transport in the Turbulent and CME-disrupted Stellar Wind of AU Microscopii
Authors: Federico Fraschetti, Julián D. Alvarado-Gómez, Jeremy J. Drake, Ofer Cohen, Cecilia Garraffo
Figure caption: Left: flux of 1 GeV protons (magnetogram from Klein et al. 2021b) impinging onto a latitudinal ring of semiaperture Δθ = 5° centered on the equatorial plane at radius R = R  b  in a quiescent wind for the strong turbulence case of σ 2 = 1. An azimuthal binning of 1° is used and the green overlayed curve is a smoothed average with a 5° smoothing width. The left-hand side y-axis provides the EP flux rescaled to the peak of the HZ planet of GJ 876 (see Section 5). The right-hand side y-axis uses a crudely approximated renormalization to the solar EP flux based on a flaring rate estimate. Right: same as the left panel but for the case of a 90 minutes post-CME eruption.
Paper: Origin of Nitrogen Isotopic Variations in the Rocky Bodies of the Solar System
Authors: Damanveer S. Grewal
Figure caption: Nitrogen isotopic compositions of cosmochemical reservoirs in the solar system. δ 15N values of bulk meteorites (chondrites, ureilites, and iron meteorites), Earth’s mantle and atmosphere, Moon and Martian mantle are distinct relative to the 15N-poor PSN and 15N-rich cometary reservoirs. Meteorites are plotted in red and blue using the NC-CC classification based on the isotopic anomalies of Cr, Ti, and Mo. Refer to Table A1 in the Appendix and the compilation of Grewal et al. (2021b) for the source of the data for the δ 15N values.
Paper: Exploring the Fate of Stellar Core Collapse with Supernova Relic Neutrinos
Authors: Yosuke Ashida, Ken'ichiro Nakazato
Figure caption: Theoretical model predictions of the SRN ﹩{\bar{\nu }}_{e}﹩ flux in the present study, in comparison with the 90% confidence level (C.L.) upper limits on the extraterrestrial ﹩{\bar{\nu }}_{e}﹩ flux from the latest experimental searches at SK (Abe et al. 2021) and KamLAND (Abe et al. 2022). The SRN ﹩{\bar{\nu }}_{e}﹩ fluxes estimated under the assumption that neutrinos originate from a single component of the SN with a canonical-mass neutron star (f HNS = 0 and f BH = 0), the SN with a high-mass neutron star (f HNS = 1 and f BH = 0), and the failed SN (f BH = 1) are shown with red, blue, and green lines, respectively. The solid and dashed lines correspond to the results for normal and inverted neutrino mass hierarchies (NH and IH), respectively. Here the fluxes with three different nuclear equations of state in Table 1 are shown in the same style. Detailed descriptions about modeling are given in Section 2.
Paper: Exploring the Fate of Stellar Core Collapse with Supernova Relic Neutrinos
Authors: Yosuke Ashida, Ken'ichiro Nakazato
Figure caption: Two-dimensional map of the integrated SRN ﹩{\bar{\nu }}_{e}﹩ flux as a function of f BH and f HNS for the cases with NH. Models with different EOSs and integration ranges of the neutrino energy, E  ν  are shown in each panel: (1a) Togashi EOS and 13.3 MeV < E  ν  < 31.3 MeV, (1b) LS220 EOS and 13.3 MeV < E  ν  < 31.3 MeV, (1c) Shen EOS and 13.3 MeV < E  ν  < 31.3 MeV, (2a) Togashi EOS and 17.3 MeV < E  ν  < 31.3 MeV, (2b) LS220 EOS and 17.3 MeV < E  ν  < 31.3 MeV, and (2c) Shen EOS and 17.3 MeV < E  ν  < 31.3 MeV. Dashed–dotted, dotted, and dashed lines represent the 2σ C.L. expected sensitivities at SK-Gd over 10 yr, HK over 3 yr, and HK over 5 yr, respectively. HK over 5 yr could test the entire parameter space at 2σ C.L. for the (1a) case.
Paper: Exploring the Fate of Stellar Core Collapse with Supernova Relic Neutrinos
Authors: Yosuke Ashida, Ken'ichiro Nakazato
Figure caption: The integrated SRN ﹩{\bar{\nu }}_{e}﹩ fluxes with E  ν  > 17.3 MeV estimated under the assumption that SRNs originate from a single component listed in Table 1. The left and right panels show the results for NH and IH, respectively. The orange solid lines and shaded regions represent the best-fit values and their ±1σ uncertainties and the red dashed–dotted lines the 90% observed upper limits from the latest SK analysis (Abe et al. 2021) associated with the spectral models in Nakazato et al. (2015). Note that the SRN flux for each component may change for various assumptions such as ﹩{M}_{\min }﹩ and BH formation model as discussed in Section 4.3.
Paper: Exploring the Fate of Stellar Core Collapse with Supernova Relic Neutrinos
Authors: Yosuke Ashida, Ken'ichiro Nakazato
Figure caption: The event rate spectra of SRN ﹩{\bar{\nu }}_{e}﹩ per 22.5 kton water per year obtained using the models of (a) Togashi EOS, (b) LS220 EOS, and (c) Shen EOS. The line and color conventions are the same as the ones used in Figure 1.
Paper: Exploring the Fate of Stellar Core Collapse with Supernova Relic Neutrinos
Authors: Yosuke Ashida, Ken'ichiro Nakazato
Figure caption: Detectable regions on the f BH–f HNS plane at SK-Gd over 10 yr for three different EOSs for NH (left) and IH (right). The colored areas represent the regions excluded from either 13.3 MeV < E  ν  < 31.3 MeV or 17.3 MeV < E  ν  < 31.3 MeV at 2σ C.L. Note that these are not statistically combined regions.
Paper: Exploring the Fate of Stellar Core Collapse with Supernova Relic Neutrinos
Authors: Yosuke Ashida, Ken'ichiro Nakazato
Figure caption: Same distributions with the 2σ C.L. expected sensitivity lines as in Figure 4 but for the cases with IH. HK over 5 yr could test the entire parameter space at 2σ C.L. for the Togashi EOS cases in (1a) and (2a).
Paper: Exploring the Fate of Stellar Core Collapse with Supernova Relic Neutrinos
Authors: Yosuke Ashida, Ken'ichiro Nakazato
Figure caption: Same distributions as Figure 7 but with a doubled amount of neutrino emission from the BH formation.
Paper: Exploring the Fate of Stellar Core Collapse with Supernova Relic Neutrinos
Authors: Yosuke Ashida, Ken'ichiro Nakazato
Figure caption: Same distributions as Figure 6 but for HK 10 yr and different C.L. Here the results with three different EOSs are shown for NH (top) and IH (bottom).
Paper: Exploring the Fate of Stellar Core Collapse with Supernova Relic Neutrinos
Authors: Yosuke Ashida, Ken'ichiro Nakazato
Figure caption: Same distributions as Figure 7 but with ﹩{M}_{\min }=8\,{M}_{\odot }﹩ in Equation (1).
Paper: The Location and Angle Distribution of Magnetic Reconnection in the Solar Corona
Authors: Kalman J. Knizhnik, Logan C. Cabral-Pelletier
Figure caption: Left: cartoon showing a field line before (purple) and after (green) reconnection. The bottom portion of the reconnecting field line is shared during the two time steps, and the spacing between the “before” and “after” field lines is defined as ds(n) along the length of the “before” field line, where n is the step number along the field line (for the same step size along the two field lines). The upper end of the green field line arrives at its location due to some imposed velocity, having at the previous time step been at the location (x 0, y 0). Right: the gradient of ds(n) will start at 0, where the two field lines share a segment, and then increase rapidly near the reconnection point, where the two field lines diverge the quickest. As the segments of the field lines beyond the reconnection event move farther apart, their separation increases, but, in the absence of additional reconnection events, the gradient of the separation will decrease and plateau at some small value.
Paper: The Location and Angle Distribution of Magnetic Reconnection in the Solar Corona
Authors: Kalman J. Knizhnik, Logan C. Cabral-Pelletier
Figure caption: Sample magnetic field lines (green) traced from the photospheric boundary at t = t 1. The contour shading (red/blue) shows the horizontal driving velocity on the photosphere. The black circle is the PIL.
Paper: The Location and Angle Distribution of Magnetic Reconnection in the Solar Corona
Authors: Kalman J. Knizhnik, Logan C. Cabral-Pelletier
Figure caption: Reconnecting field lines shown before and after reconnection. The red and blue field lines reconnect between time steps t = t 1 and t = t 2 and form the orange field line, which shares a seed point with the blue field line at both time steps. The black dot and star identify the location of the reconnection as determined from the bifurcation and closest-distance approaches, respectively.
Paper: The Location and Angle Distribution of Magnetic Reconnection in the Solar Corona
Authors: Kalman J. Knizhnik, Logan C. Cabral-Pelletier
Figure caption: Histograms of the reconnection angles from the bifurcation (top) and minimum separation (bottom) methods. The median reconnection angle is shown with the red vertical line.
Paper: The Location and Angle Distribution of Magnetic Reconnection in the Solar Corona
Authors: Kalman J. Knizhnik, Logan C. Cabral-Pelletier
Figure caption: Actual displacements of the driven ends  r   i  of only the reconnecting field lines, starting at seed points  r   o  mapped onto  r   o . The reconnecting field lines satisfy the condition of Equation (3.4).
Paper: The Location and Angle Distribution of Magnetic Reconnection in the Solar Corona
Authors: Kalman J. Knizhnik, Logan C. Cabral-Pelletier
Figure caption: Expected (top) and actual (bottom) displacements of the driven ends  r   i  of the field lines, starting at seed points  r   o  mapped to the locations of  r   o .
Paper: The Location and Angle Distribution of Magnetic Reconnection in the Solar Corona
Authors: Kalman J. Knizhnik, Logan C. Cabral-Pelletier
Figure caption: Calculation of the bifurcation method from the field lines plotted in the bottom right panel of Figure 7. The separation between the field line before and after reconnection, ds (red), is plotted along with the gradient of ds (blue). The location of the reconnection is identified at the location of maximum gradient (black line).
Paper: The Location and Angle Distribution of Magnetic Reconnection in the Solar Corona
Authors: Kalman J. Knizhnik, Logan C. Cabral-Pelletier
Figure caption: Top: B ph(r) given by Equation (2.6). Bottom: contour plot of B ph(r) at the photosphere of the simulation.