adsabs/AstroCLIMB huggingface dataset:
Paper: A Comprehensive Study of Open Cluster Chemical Homogeneity Using APOGEE and Milky Way Mapper Abundances
Authors: Amaya Sinha, Gail Zasowski, Peter Frinchaboy, Katia Cunha, Diogo Souto, Jamie Tayar, Keivan Stassun
Figure caption: Top: [Mg/Fe] uncertainties calculated using stars with multiple visits. Middle: [Mg/Fe] uncertainties calculated by ASPCAP for DR17. Bottom: the subtracted difference between the uncertainties calculated using multiple visits and the uncertainties from ASPCAP.
Paper: A Comprehensive Study of Open Cluster Chemical Homogeneity Using APOGEE and Milky Way Mapper Abundances
Authors: Amaya Sinha, Gail Zasowski, Peter Frinchaboy, Katia Cunha, Diogo Souto, Jamie Tayar, Keivan Stassun
Figure caption: Left: a plot of the [Mg/Fe] vs. [Fe/H] plane where the full giant-star sample in APOGEE DR17 (subject to the same quality cuts as in Section 2.1.3) is shown in black, and the clusters are colored by log(age). Right: the guiding radius and galactocentric height of all the clusters in our sample, colored by the number of member stars as described in Section 2.2.1.
Paper: A Comprehensive Study of Open Cluster Chemical Homogeneity Using APOGEE and Milky Way Mapper Abundances
Authors: Amaya Sinha, Gail Zasowski, Peter Frinchaboy, Katia Cunha, Diogo Souto, Jamie Tayar, Keivan Stassun
Figure caption: The literature comparison plots for the well-studied OCs in our sample using IPL-3 ASPCAP (colored in magenta). The horizontal line indicates the median 99.7% confidence limit for that cluster’s homogeneity.
Paper: Electron Acceleration in Magnetic Islands in Quasi-parallel Shocks
Authors: N. Bessho, L.-J. Chen, M. Hesse, J. Ng, L. B. Wilson, J. E. Stawarz, H. Madanian
Figure caption: (a) W  H  (red), W  m,E×B  (blue), W non (green), and W  z−sum = W  m,E×B  + W non (magenta) as a function of ∣θ∣, for a case of symmetric E  H . E non = [3/(4π)]E  HR (V is/〈v  z 〉). (b) Schematic of asymmetric E  H , where E  HR  = E  H1 in Region 1 and E  HR  = E  H2 in Region 2. (c) and (d) W  H , W  m,E×B , W non, and W  z−sum for asymmetric E  H . E non = [3/(4π)]E  H1(V is/〈v  z−av〉), and E  H1 = 4E  H2. In (c), 〈v  z1〉 = (3/2)〈v  z−av〉 and 〈v  z2〉 = (1/2)〈v  z−av〉, while in (d), 〈v  z1〉 = (8/3)〈v  z−av〉 and 〈v  z2〉 = − (2/3)〈v  z−av〉.
Paper: Electron Acceleration in Magnetic Islands in Quasi-parallel Shocks
Authors: N. Bessho, L.-J. Chen, M. Hesse, J. Ng, L. B. Wilson, J. E. Stawarz, H. Madanian
Figure caption: (a) 〈v  d 〉 in Equation (A10) as a function of k. (b) (Red): 〈v  d 〉 in Equation (A26) as a function of s. (Blue): grad-B drift. The difference between the red curve and the blue curve represents Δ v . (c) Schematic of electric field E  mz  in the radial direction. The red circle represents an electron’s gyroorbit whose center is at r = R.
Paper: Electron Acceleration in Magnetic Islands in Quasi-parallel Shocks
Authors: N. Bessho, L.-J. Chen, M. Hesse, J. Ng, L. B. Wilson, J. E. Stawarz, H. Madanian
Figure caption: (a)–(d) Electron trajectory (red) trapped in island 1, and magnetic field B  z  (color). (e)–(f) Lorentz factor γ and work for the electron. Same format as in Figure 2.
Paper: Electron Acceleration in Magnetic Islands in Quasi-parallel Shocks
Authors: N. Bessho, L.-J. Chen, M. Hesse, J. Ng, L. B. Wilson, J. E. Stawarz, H. Madanian
Figure caption: (a) Island betatron acceleration. An electron (magenta) is gyrating around a local field. Counterclockwise electric field (green) appears when ∂B  z /∂t < 0. (b) Electron trajectory (blue+red) trapped in island 1. The red time interval (starting from and ending at the green dot, and numbered from 1 to 14) shows a closed chaotic motion. (c) Scatter plot for Equation (10) for electrons accelerated in island 1. Red: electron showing a loop trajectory. Black: a chaotic motion. When an electron shows multiple closed trajectories, each closed trajectory is shown as a separate cross.
Paper: Electron Acceleration in Magnetic Islands in Quasi-parallel Shocks
Authors: N. Bessho, L.-J. Chen, M. Hesse, J. Ng, L. B. Wilson, J. E. Stawarz, H. Madanian
Figure caption: (a) Flux rope moving in x with a speed V  is . The Hall electric field points toward the island center, and the nonideal electric field points to the negative z direction. (b) Top view and the motional electric field.
Paper: Determining the Extents, Geometries, and Kinematics of Narrow-line Region Outflows in Nearby Seyfert Galaxies
Authors: Garrett E. Polack, Mitchell Revalski, D. Michael Crenshaw, Travis C. Fischer, Henrique R. Schmitt, Steven B. Kraemer, Beena Meena, Marc Rafelski
Figure caption: The radial extent of the [O III] gas (R [O III]) vs. [O III] luminosity (L [O III]) for the 12 targets in this study (colored squares), the five targets from M. Revalski et al. (2021; black squares), and the archival targets used to determine a fixed threshold for image analysis (gray circles). The green plusses indicate the values of our 12 targets that were measured using the standardized 3σ flux contour of 2.034 × 10−17, demonstrating where these AGN would lie in this parameter space with a shallower threshold closer to those used by the literature studies. The three lines show the best fits to the targets in our study using their individual 3σ thresholds (solid purple, 0.39), the same targets using the fixed contour limit (solid green, 0.62), and the archival AGN using an adopted line equation from (T. Storchi-Bergmann et al. 2018; gray dashed, 0.51). As discussed in the text, the radial extents for our targets are larger because the deep imaging reaches fainter emission than some earlier studies.
Paper: Determining the Extents, Geometries, and Kinematics of Narrow-line Region Outflows in Nearby Seyfert Galaxies
Authors: Garrett E. Polack, Mitchell Revalski, D. Michael Crenshaw, Travis C. Fischer, Henrique R. Schmitt, Steven B. Kraemer, Beena Meena, Marc Rafelski
Figure caption: Kinematic plot examples for six targets. Each plot is composed of three vertical sections, velocity (top), FWHM (middle), and flux (Log(erg s−1 cm−2)) (bottom). The x-axis shows distance across the slit, with the zero-point established by the brightness centroid of the AGN, and positive x-values indicating direction along of the position angle of the slit. For NGC 788, NGC 1667, and IC 3639, positive x-values indicate a southward direction on the sky, and for NGC 3393, NGC 7682, and UGC 1395, positive x-values indicate a northward direction. Each slit bin has either one, two, or three associated components output from the fitting routine, sorted by flux into high (blue circles), medium (red squares), or low flux (green triangles) components. Positive velocity indicates redshifted components, and negative values indicate blueshifted components.
Paper: Determining the Extents, Geometries, and Kinematics of Narrow-line Region Outflows in Nearby Seyfert Galaxies
Authors: Garrett E. Polack, Mitchell Revalski, D. Michael Crenshaw, Travis C. Fischer, Henrique R. Schmitt, Steven B. Kraemer, Beena Meena, Marc Rafelski
Figure caption: Hα velocity plots for the six targets whose slits encompass the majority of their ionized gas structures. The x-axis for each target is converted to deprojected distances in parsecs within the disk, using the spatial scales from Table 1. Both boundary methods have been applied. The boundaries based on observed velocities and FWHM (3.5.1) are symmetric vertical lines, with magenta indicating the extent of the disturbed gas, and cyan indicating the extent of the outflow components, if present. The horizontal green band represents the bounds of V proj. Components in this region are observed values, as they are considered rotational, while components outside are deprojected to their “true” spatial velocities assuming they are outflowing within the disk. See Equations (2) and (3) for the deprojection methodology.
Paper: Determining the Extents, Geometries, and Kinematics of Narrow-line Region Outflows in Nearby Seyfert Galaxies
Authors: Garrett E. Polack, Mitchell Revalski, D. Michael Crenshaw, Travis C. Fischer, Henrique R. Schmitt, Steven B. Kraemer, Beena Meena, Marc Rafelski
Figure caption: An example of the Gaussian fitting results for the Hα λ6563 and [N II] λ λ 6548,6583 emission lines for one bin along the G750M observation for NGC 7682. Observed wavelengths are on the x-axis, and flux is on the y-axis. Two sets of gray vertical dashed lines indicate the regions used to determine the continuum level (horizontal gray line). The thick black line indicates the original spectral data, while the magenta line shows the combined fit for all emission-line components. In this case, the fitting routine found that two kinematic components were optimal to fit each line profile: a wider, redshifted component with a lower peak flux (orange) and a narrower, blueshifted component with a higher peak flux (blue).
Paper: Determining the Extents, Geometries, and Kinematics of Narrow-line Region Outflows in Nearby Seyfert Galaxies
Authors: Garrett E. Polack, Mitchell Revalski, D. Michael Crenshaw, Travis C. Fischer, Henrique R. Schmitt, Steven B. Kraemer, Beena Meena, Marc Rafelski
Figure caption: Results from the elliptical modeling of the ground-based images detailed in Section 3.2. The left panel shows the ground-based images, the center panel shows the reconstructed model of the galaxy using the isophotal ellipses fit to the image, and the right panel shows the residual from the model subtraction. The axes give the pixel count, with each image showing a 100″ × 100″ field of view, except for NGC 1358, NGC 2273, NGC 3393, and NGC 5427, which have a 150″ × 150″ FOV in order to fit their extended structures.
Paper: Determining the Extents, Geometries, and Kinematics of Narrow-line Region Outflows in Nearby Seyfert Galaxies
Authors: Garrett E. Polack, Mitchell Revalski, D. Michael Crenshaw, Travis C. Fischer, Henrique R. Schmitt, Steven B. Kraemer, Beena Meena, Marc Rafelski
Figure caption:                         The NGC 3393 WFC3 continuum-subtracted [O III] image using data from HST Program ID: 12365 (PI: J. Wang, see also W. P. Maksym et al. 2016, 2017, 2019). Data reduction was performed using the same methods outlined in Section 2.1, and keeps the same 10″ × 10″ aspect ratio as the images from Figure 2. The HST STIS slit (PA: 39.°98) is overlaid on the image as the white shaded region running SW to NE.
Paper: Solar Vortex Tubes. III. Vorticity and Energy Transport
Authors: Suzana S. A. Silva, Gary Verth, Istvan Ballai, Erico L. Rempel, Sergiy Shelyag, Luiz A. C. A. Schiavo, Tiago F. P. Gomes, Viktor Fedun
Figure caption: Close view of the simulation box at t = 0 s. For z ≤ 1.0, the surface is colored by the z-component of the velocity field. The velocity field lines are shown in orange and green and were traced from points within the vortex boundary for every vortex detected at t = 0 s. The green velocity fields indicate the selected vortices. The red (blue) areas depict regions where the temperature ranges from 5500 to 6000 K (2080–3500 K).
Paper: Solar Vortex Tubes. III. Vorticity and Energy Transport
Authors: Suzana S. A. Silva, Gary Verth, Istvan Ballai, Erico L. Rempel, Sergiy Shelyag, Luiz A. C. A. Schiavo, Tiago F. P. Gomes, Viktor Fedun
Figure caption: Average temperature at the vortex center as a function of height. The red lines are for the initial time t0 = 0, the green lines are for t1 = 20 s, and the blue lines are for t2 = 40 s. (a)–(i) Temperature at the center of the detected cold vortices; (j) the temperature is normalized by the temperature at the base of the vortex, T  b , and the height, h, is subtracted by h 0, which is the distance from the base of the vortex to the simulated surface, and normalized by the vertical length of the vortex, L.
Paper: Solar Vortex Tubes. III. Vorticity and Energy Transport
Authors: Suzana S. A. Silva, Gary Verth, Istvan Ballai, Erico L. Rempel, Sergiy Shelyag, Luiz A. C. A. Schiavo, Tiago F. P. Gomes, Viktor Fedun
Figure caption: The average T1, T2, T3, and T4 terms normalized by T3 along the vortex radius from the center, r = 0, to the boundary r = R. The radial profiles are shown for vortices #7 (a), (d), (g), #8 (b), (e), (h), and #12 (c), (f), (i) at different heights: H = 0.1 Mm (a), (b), (c); H = 0.3 Mm (d), (e), (f); H = 0.5 Mm (g), (h), (i).
Paper: Solar Vortex Tubes. III. Vorticity and Energy Transport
Authors: Suzana S. A. Silva, Gary Verth, Istvan Ballai, Erico L. Rempel, Sergiy Shelyag, Luiz A. C. A. Schiavo, Tiago F. P. Gomes, Viktor Fedun
Figure caption: The average density, temperature, and pressure along the vortex radius from the center, r = 0, to the boundary r = R. The radial profiles are shown for vortices #7 (a), (d), (g), #8 (b), (e), (h), and #12 (c), (f), (i) at different heights: H = 0.1 Mm (a), (b), (c); H = 0.3 Mm (d), (e), (f); and H = 0.5 Mm (g), (h), (i).
Paper: On the Physical Nature of Lyα Transmission Spikes in High-redshift Quasar Spectra
Authors: Hanjue Zhu, 涵珏 朱, Nickolay Y. Gnedin, Camille Avestruz
Figure caption: Univariate functions at z = 5.25 from the intermediate reionization case. There is an apparent anticorrelation between flux and n  b , and positive correlations between flux and ﹩{{ \mathcal F }}_{\nu }﹩, T, and ﹩{{ \mathcal G }}_{\nu }﹩, respectively. These trends suggest that Lyα transmission spikes are predominately found in regions of lower density, higher ionization, and higher temperatures.
Paper: Solar Vortex Tubes. III. Vorticity and Energy Transport
Authors: Suzana S. A. Silva, Gary Verth, Istvan Ballai, Erico L. Rempel, Sergiy Shelyag, Luiz A. C. A. Schiavo, Tiago F. P. Gomes, Viktor Fedun
Figure caption: Same as Figure 3, but here, we show the results for the hot vortices.
Paper: On the Physical Nature of Lyα Transmission Spikes in High-redshift Quasar Spectra
Authors: Hanjue Zhu, 涵珏 朱, Nickolay Y. Gnedin, Camille Avestruz
Figure caption: Baryon and H I number densities (top) and ﹩{{ \mathcal F }}_{\nu }﹩ (bottom) along a random LOS. ﹩{{ \mathcal F }}_{\nu }﹩ shows an anticorrelation with density, albeit not a strong one.
Paper: On the Physical Nature of Lyα Transmission Spikes in High-redshift Quasar Spectra
Authors: Hanjue Zhu, 涵珏 朱, Nickolay Y. Gnedin, Camille Avestruz
Figure caption: Bivariate functions at z = 5.25 from the intermediate reionization case.
Paper: Asteroseismology of the Nearby K Dwarf σ Draconis Using the Keck Planet Finder and TESS
Authors: Marc Hon, Daniel Huber, Yaguang Li, Travis S. Metcalfe, Timothy R. Bedding, Joel Ong, Ashley Chontos, Ryan Rubenzahl, Samuel Halverson, Rafael A. García, Hans Kjeldsen, Dennis Stello, Daniel R. Hey, Tiago Campante, Andrew W. Howard, Steven R. Gibson, Kodi Rider, Arpita Roy, Ashley D. Baker, Jerry Edelstein, Chris Smith, Benjamin J. Fulton, Josh Walawender, Max Brodheim, Matt Brown, Dwight Chan, Fei Dai, William Deich, Colby Gottschalk, Jason Grillo, Dave Hale, Grant M. Hill, Bradford Holden, Aaron Householder, Howard Isaacson, Yuzo Ishikawa, Sharon R. Jelinsky, Marc Kassis, Stephen Kaye, Russ Laher, Kyle Lanclos, Chien-Hsiu Lee, Scott Lilley, Ben McCarney, Timothy N. Miller, Joel Payne, Erik A. Petigura, Claire Poppett, Michael Raffanti, Constance Rockosi, Dale Sanford, Christian Schwab, Abby P. Shaum, Martin M. Sirk, Roger Smith, Jim Thorne, John Valliant, Adam Vandenberg, Shin Ywan Wang, Edward Wishnow, Truman Wold, Sherry Yeh, Ashley Baker, Sarbani Basu, Megan Bedell, Heather M. Cegla, Ian Crossfield, Courtney Dressing, Xavier Dumusque, Heather Knutson, Dimitri Mawet, John O'Meara, Guđmundur Stefánsson, Johanna Teske, Gautam Vasisht, Sharon Xuesong Wang, Lauren M. Weiss, Joshua N. Winn, Jason T. Wright
Figure caption: Radius vs. effective temperature of low-mass dwarf and subgiant stars with detected solar-like oscillations. σ Dra is the coolest dwarf star to have solar-like oscillations detected using TESS photometry to date. Only several cool dwarfs currently have solar-like oscillations detected from photometry, including Kepler-444 (T. L. Campante et al. 2015). Also shown is ϵ Ind, the coolest star with detected solar-like oscillations, but only from RV observations (T. L. Campante et al. 2024). Also shown are other dwarfs and subgiants with solar-like oscillations observed by TESS (E. Hatt et al. 2023), by the Kepler mission (A. Serenelli et al. 2017; M. N. Lund et al. 2017; V. Silva Aguirre et al. 2017), and by the K2 mission (W. J. Chaplin et al. 2015; M. N. Lund et al. 2016; L. González-Cuesta et al. 2023; M. N. Lund et al. 2024). Highlighted are several dwarf stars for which solar-like oscillations have been detected and analyzed using space-based photometry—α Men (A. Chontos et al. 2021), 16 Cyg A/B (T. S. Metcalfe et al. 2012), λ 2 For (M. B. Nielsen et al. 2020), π Men, γ Pav, ζ Tuc (D. Huber et al. 2022), ρ CrB (T. S. Metcalfe et al. 2021), λ Ser (T. S. Metcalfe et al. 2023), and HD 102365. Radii and effective temperatures in the plot are adopted from the TESS Input Catalog (STScI 2018, DOI: 10.17909/fwdt-2x66), with MIST solar-metallicity evolutionary tracks (J. Choi et al. 2016) displayed in the background.
Paper: Asteroseismology of the Nearby K Dwarf σ Draconis Using the Keck Planet Finder and TESS
Authors: Marc Hon, Daniel Huber, Yaguang Li, Travis S. Metcalfe, Timothy R. Bedding, Joel Ong, Ashley Chontos, Ryan Rubenzahl, Samuel Halverson, Rafael A. García, Hans Kjeldsen, Dennis Stello, Daniel R. Hey, Tiago Campante, Andrew W. Howard, Steven R. Gibson, Kodi Rider, Arpita Roy, Ashley D. Baker, Jerry Edelstein, Chris Smith, Benjamin J. Fulton, Josh Walawender, Max Brodheim, Matt Brown, Dwight Chan, Fei Dai, William Deich, Colby Gottschalk, Jason Grillo, Dave Hale, Grant M. Hill, Bradford Holden, Aaron Householder, Howard Isaacson, Yuzo Ishikawa, Sharon R. Jelinsky, Marc Kassis, Stephen Kaye, Russ Laher, Kyle Lanclos, Chien-Hsiu Lee, Scott Lilley, Ben McCarney, Timothy N. Miller, Joel Payne, Erik A. Petigura, Claire Poppett, Michael Raffanti, Constance Rockosi, Dale Sanford, Christian Schwab, Abby P. Shaum, Martin M. Sirk, Roger Smith, Jim Thorne, John Valliant, Adam Vandenberg, Shin Ywan Wang, Edward Wishnow, Truman Wold, Sherry Yeh, Ashley Baker, Sarbani Basu, Megan Bedell, Heather M. Cegla, Ian Crossfield, Courtney Dressing, Xavier Dumusque, Heather Knutson, Dimitri Mawet, John O'Meara, Guđmundur Stefánsson, Johanna Teske, Gautam Vasisht, Sharon Xuesong Wang, Lauren M. Weiss, Joshua N. Winn, Jason T. Wright
Figure caption: Solar-like oscillations of σ Dra as observed from 14 sectors of TESS photometry (2021 July to 2023 January). (a) The power spectral density of the star smoothed with 3 μHz wide boxcar filter. (b) The replicated échelle diagram of the smoothed power spectrum (T. R. Bedding 2012). (c) The collapsed replicated échelle diagram. The dashed line in panels (b) and (c) corresponds to Δν = 182.25 μHz, and the numbers identify the l = 0 and l = 1 mode sequences.
Paper: Exploring the Magnetic and Thermal Evolution of a Coronal Jet
Authors: Sushree S. Nayak, Samrat Sen, Arpit Kumar Shrivastav, R. Bhattacharyya, P. S. Athiray
Figure caption: Panel (a): The plot shows the variation of volume-averaged total current density (∣ J ∣), z-component of ∣ J ∣, ∣ J ∣/∣ B ∣, and J trans or ﹩\sqrt{(}{J}_{x}^{2}+{J}_{y}^{2})﹩ in solid, dotted, dashed, and dash-dot lines, respectively, over the whole computational box. Panel (b): The plot shows the variation of the above parameters near the jet base region. Panel (c): We plot all the above parameters near the bright point. The difference in the variation of J  z  is noticeable from all the plots, whereas ∣ J ∣ and ∣ J ∣/∣ B ∣ are displaying an overall decreasing trend throughout the evolution. J trans is apparently following the trend similar to ∣ J ∣ in every case.
Paper:  pop-cosmos: Scaleable Inference of Galaxy Properties and Redshifts with a Data-driven Population Model
Authors: Stephen Thorp, Justin Alsing, Hiranya V. Peiris, Sinan Deger, Daniel J. Mortlock, Boris Leistedt, Joel Leja, Arthur Loureiro
Figure caption: Photometric redshift vs. spectroscopic redshift for ∼12,000 COSMOS galaxies using pop-cosmos (Section 2.1.2; J. Alsing et al. 2024), Prospector-α (Section 2.1.1; J. Leja et al. 2017, 2018, 2019a, 2019b), LePhare (S. Arnouts et al. 1999; O. Ilbert et al. 2006, 2009), and EAZY (G. B. Brammer et al. 2008). Results for pop-cosmos and Prospector are from this work; plotted points are posterior medians and 68% credible intervals. Results for LePhare and EAZY are from J. R. Weaver et al. (2022); plotted points are posterior medians for LePhare and MAP estimates for EAZY. Error bars show the reported 68% confidence levels for both codes. The threshold of ∣Δ z ∣ > 0.15 is indicated on all panels with dashed gray lines, where Δ z  = (z − z spec)/(1 + z spec). Galaxies where ∣Δ z ∣ > 0.15 are indicated with more solid markers. Galaxies that are only outlying for one of the codes are shown with black circles.
Paper: Exploring the Magnetic and Thermal Evolution of a Coronal Jet
Authors: Sushree S. Nayak, Samrat Sen, Arpit Kumar Shrivastav, R. Bhattacharyya, P. S. Athiray
Figure caption: Variation of volume-averaged magnetic energy density and kinetic energy density normalized over total energy density (a) over the whole computational volume, (b) near the jet base region, and (c) in the neighborhood of the bright point region during the evolution. The dissipation in the magnetic energy by reconnection while feeding the kinetic energy, during the initial time of the simulation, is evident in every panel. Later kinetic energy is also dissipated by the action of viscous relaxation. This feedback relationship is significant in the jet region and more in the bright point region. This suggests a higher rate of dissipation of magnetic energy and conversion to kinetic energy near the locality of the jet base region and the bright point location.
Paper:  pop-cosmos: Scaleable Inference of Galaxy Properties and Redshifts with a Data-driven Population Model
Authors: Stephen Thorp, Justin Alsing, Hiranya V. Peiris, Sinan Deger, Daniel J. Mortlock, Boris Leistedt, Joel Leja, Arthur Loureiro
Figure caption: Statistics comparing the different photometric redshift estimates to spectroscopic redshifts for the ∼12,000 COSMOS galaxies (see also Figure 2 in B. Leistedt et al. 2023). Left column shows the statistics in bins of r-band magnitude; right column shows bins of z spec. All statistics are computed for Δ z  = (z − z spec)/(1 + z spec).
Paper: Exploring the Magnetic and Thermal Evolution of a Coronal Jet
Authors: Sushree S. Nayak, Samrat Sen, Arpit Kumar Shrivastav, R. Bhattacharyya, P. S. Athiray
Figure caption: Evolution of average of twist density normalized to initial value for (a) the whole computational volume in a solid line, (b) the jet base region in dotted lines, and (c) in the neighborhood of the bright point region in dashed lines during the evolution.
Paper: Exploring the Magnetic and Thermal Evolution of a Coronal Jet
Authors: Sushree S. Nayak, Samrat Sen, Arpit Kumar Shrivastav, R. Bhattacharyya, P. S. Athiray
Figure caption: Panel (a)–(d): evolution of the bald patch; field lines colored in white near the bright point structure and the subsequent flare ribbons. We have overplotted the 304 Å channel in the background. The yellow and blue contours represent the positive and negative polarities, respectively. Panel (a1)–(d1): evolution of Q factor near the bald patch for the same time period. The reconnection near the bald patch where the field lines are changing the connectivities is evident.
Paper: Exploring the Magnetic and Thermal Evolution of a Coronal Jet
Authors: Sushree S. Nayak, Samrat Sen, Arpit Kumar Shrivastav, R. Bhattacharyya, P. S. Athiray
Figure caption: Variation of average of Lorentz force normalized to initial value for (a) the whole computational volume in a solid line, (b) the jet base region in dotted lines, and (c) in the neighborhood of the bright point region in dashed lines during the evolution.
Paper: Exploring the Magnetic and Thermal Evolution of a Coronal Jet
Authors: Sushree S. Nayak, Samrat Sen, Arpit Kumar Shrivastav, R. Bhattacharyya, P. S. Athiray
Figure caption: Variation of average of free energy normalized to initial value for (a) the whole computational volume in a solid line, (b) the jet base region in dotted lines, and (c) in the neighborhood of the bright point region in dashed lines during the evolution.