adsabs/AstroCLIMB huggingface dataset:
Paper: oMEGACat. VII. Tracing Interstellar and Intracluster Medium of ω Centauri Using Sodium Absorptions
Authors: Z. Wang, 梓先 王, A. C. Seth, M. Latour, J. Strader, M. Häberle, N. Neumayer, C. Clontz, S. Kamann, M. S. Nitschai, M. Alfaro-Cuello, A. Bellini, A. Feldmeier-Krause, M. Libralato, A. P. Milone, P. J. Smith, S. O. Souza, G. van de Ven
Figure caption: Reddening (E) as a function of distance for stars within 1° of the ω Cen from Gaia DR3. Stars are color-coded by their angular distance to the center of ω Cen. The gray line and shaded region represent the median and (16th, 84th) percentiles. The reddening and distance values are derived from Gaia BP/RP spectra using a machine learning method (X. Zhang et al. 2023). The distance and measured reddening of ω Cen are denoted by a red star marker. This figure indicates that the ISM is primarily located at distances between 0 and 2 kpc. Therefore, the foreground ISM is unlikely to interact with ω Cen.
Paper: oMEGACat. VII. Tracing Interstellar and Intracluster Medium of ω Centauri Using Sodium Absorptions
Authors: Z. Wang, 梓先 王, A. C. Seth, M. Latour, J. Strader, M. Häberle, N. Neumayer, C. Clontz, S. Kamann, M. S. Nitschai, M. Alfaro-Cuello, A. Bellini, A. Feldmeier-Krause, M. Libralato, A. P. Milone, P. J. Smith, S. O. Souza, G. van de Ven
Figure caption: Correlation between the dispersion measure and interpolated EWD2,ISM from the Voronoi-binned map (right panel of Figure 4), using the dispersion measures and coordinates of 18 pulsars (W. Chen et al. 2023; S. Dai et al. 2023). This figure shows a strong correlation between the dispersion measure and foreground Na atomic gas, indicating that it is inappropriate to attribute the dispersion measure variation solely to intracluster ionized gas.
Paper: oMEGACat. VII. Tracing Interstellar and Intracluster Medium of ω Centauri Using Sodium Absorptions
Authors: Z. Wang, 梓先 王, A. C. Seth, M. Latour, J. Strader, M. Häberle, N. Neumayer, C. Clontz, S. Kamann, M. S. Nitschai, M. Alfaro-Cuello, A. Bellini, A. Feldmeier-Krause, M. Libralato, A. P. Milone, P. J. Smith, S. O. Souza, G. van de Ven
Figure caption: Width of horizontal branch (y-axis) from Na I D-corrected photometry in different relative reddening rescaling factors and Voronoi-binning S/N. The solid line represents the HB width from uncorrected photometry in H24. The dashed line shows the HB width after applying the corrections from H24. Colored lines indicate HB widths after correcting the photometry with our Na I D-inferred relative reddening scaled by various factors. This figure demonstrates that applying a rescaling factor of 0.1 to our Na I D-inferred reddening yields an HB width comparable to that obtained from H24 ’s correction.
Paper: oMEGACat. VII. Tracing Interstellar and Intracluster Medium of ω Centauri Using Sodium Absorptions
Authors: Z. Wang, 梓先 王, A. C. Seth, M. Latour, J. Strader, M. Häberle, N. Neumayer, C. Clontz, S. Kamann, M. S. Nitschai, M. Alfaro-Cuello, A. Bellini, A. Feldmeier-Krause, M. Libralato, A. P. Milone, P. J. Smith, S. O. Souza, G. van de Ven
Figure caption: Spectral fitting of the stacked spectrum from all warm HB stars with S/N > 40 pix−1 and Teff > 10,000 K. The definitions of the colors of each line and region are consistent with those in Figure 3. This figure primarily investigates the presence of Na I D absorption attributed to the intracluster gas of ω Cen. Based on the EW of D1 line (right-most absorption), no significant amount of intracluster Na atomic gas is detected.
Paper: Backmapping of the High- and Low-latitude Solar Wind under Multiple Heliospheric and Coronal Magnetic Field Configurations
Authors: Xinyi Ma, Liping Yang, Xueshang Feng, Hui Tian, Honghong Wu, Fang Shen, Wangning Zhang, Mengxuan Ma, Xiao Zhang, Ziwei Wang
Figure caption: Predicted HMFs by the Parker and Fisk models with in situ measurements obtained from the Ulysses (A), (B), (C), (D), and Wind (E), (F), (G), (H). Panels (A) and (E): agreement (orange) and disagreement (green) between measured and predicted HMF polarity. Panels (B) and (F): Black dots and light green dots denote one-hour cadence and filtered measured magnetic field strength, respectively; pink dots and light sky blue dots show the predicted magnetic field strength by the Parker and Fisk models, respectively. Panels (C) and (G): observed (circular markers) and predicted values (red dotted line for Parker and blue dotted line for Fisk) of Bθ*r0/Br*r (where r0 = 1 au and r is the heliocentric distance), representing the meridional magnetic field component Bθ divided by the radial magnetic field component Br. Panels (D) and (H): same as panels (C) and (G), but for the azimuthal field component (Bϕ).
Paper: Backmapping of the High- and Low-latitude Solar Wind under Multiple Heliospheric and Coronal Magnetic Field Configurations
Authors: Xinyi Ma, Liping Yang, Xueshang Feng, Hui Tian, Honghong Wu, Fang Shen, Wangning Zhang, Mengxuan Ma, Xiao Zhang, Ziwei Wang
Figure caption: Backmapping of the solar wind measured by the Ulysses and Wind spacecraft to the source surface of the PFSS model (2.5R⊙) based on the Parker and Fisk HMF model. Panel (A): examples of Parker (red) and Fisk (blue) magnetic field lines traced from identical measurement points to r = 2.5R⊙. Panel (B): magnetic footpoints at 2.5R⊙ traced from measurements by Ulysses (solid markers) and Wind (hollow markers) using the Parker (circles) and Fisk (triangles) models. Color coding indicates polarity: olive for negative, magenta for positive, and black dotted lines for neutral line. Panel (C): latitudinal (Δθ) and longitudinal (Δϕ) deviations between Parker and Fisk magnetic footpoints at r = 2.5R⊙, traced from Ulysses measurements. The color encodes the count. The blue and red lines overlaid on the histograms represent the smoothed probability density distributions of the deviation values, derived from kernel density estimation. Panel (D): same as panel (C), but for Wind measurements.
Paper: Backmapping of the High- and Low-latitude Solar Wind under Multiple Heliospheric and Coronal Magnetic Field Configurations
Authors: Xinyi Ma, Liping Yang, Xueshang Feng, Hui Tian, Honghong Wu, Fang Shen, Wangning Zhang, Mengxuan Ma, Xiao Zhang, Ziwei Wang
Figure caption: Backmapping of the solar wind measured by the Ulysses and Wind spacecraft from the source surface (2.5R⊙) to the photosphere based on the Fisk HMF model. Panel (A): representative magnetic field lines from the PFSS (pink), PFCS (dark violet), and CSSS (medium sea green) CMF models. Panels (B) and (C): corresponding photospheric footpoints traced from the Ulysses (B) and Wind (C) in situ observations, overlaid on a synoptic magnetogram, respectively. Panel (D): view of the Sun’s north pole created by reprojecting the STEREO-A/SECCHI EUVI 195 Å synoptic map onto a spherical coordinate system, with backmapped solar wind source regions color coded by speed during Ulysses’ midlatitude scan. Panel (E): same as panel (D), but for Wind measurements.
Paper: Backmapping of the High- and Low-latitude Solar Wind under Multiple Heliospheric and Coronal Magnetic Field Configurations
Authors: Xinyi Ma, Liping Yang, Xueshang Feng, Hui Tian, Honghong Wu, Fang Shen, Wangning Zhang, Mengxuan Ma, Xiao Zhang, Ziwei Wang
Figure caption: Latitudinal (Δθ) and longitudinal (Δϕ) deviations of photospheric footpoints among the PFSS, PFCS, and CSSS models for Ulysses measurements. Representative magnetic field lines traced from identical points at the model outer boundaries to the photosphere are included for contextual comparison.
Paper: Backmapping of the High- and Low-latitude Solar Wind under Multiple Heliospheric and Coronal Magnetic Field Configurations
Authors: Xinyi Ma, Liping Yang, Xueshang Feng, Hui Tian, Honghong Wu, Fang Shen, Wangning Zhang, Mengxuan Ma, Xiao Zhang, Ziwei Wang
Figure caption: Backmapped source regions of the Wind-measured solar wind superimposed on an EUVI synoptic image.
Paper: Backmapping of the High- and Low-latitude Solar Wind under Multiple Heliospheric and Coronal Magnetic Field Configurations
Authors: Xinyi Ma, Liping Yang, Xueshang Feng, Hui Tian, Honghong Wu, Fang Shen, Wangning Zhang, Mengxuan Ma, Xiao Zhang, Ziwei Wang
Figure caption: The same as Figure 5, but for Wind measurements.
Paper: Monitoring of 3C 286 with ALMA, IRAM, and SMA from 2006 to 2025: Stability, Synchrotron Ages, and Frequency-dependent Polarization Attributed to Core-shift
Authors: Minchul Kam, Hiroshi Nagai, Motoki Kino, Keiichi Asada, Rüdiger Kneissl, Iván Agudo, Sascha Trippe, Seiji Kameno, Ioannis Myserlis, Ramprasad Rao, Hojin Cho, Richard A. Perley, Bryan J. Butler, Mark Gurwell, Tomoki Matsuoka, Jongho Park, Carolina Casadio, Baltasar Vila Vilaro, Celia Verdugo, Matias Radiszcz, Kurt Plarre, Wanchaloem Khwammai, Diego Álvarez-Ortega, Juan Escudero, Clemens Thum, Garrett Keating
Figure caption: The spectral flux density of 3C 286 between 1 and 229 GHz. The black and magenta data points show the total flux measured with VLA (R. A. Perley & B. J. Butler 2013a) and IRAM, respectively. The gray and magenta dashed lines show the best-fit to the total flux measured with VLA and IRAM, respectively. The black and gray arrows on the x-axis indicates the break frequency at 67.2 GHz and a potential break frequency at 3.6 GHz (see Section 4.2), respectively.
Paper: Monitoring of 3C 286 with ALMA, IRAM, and SMA from 2006 to 2025: Stability, Synchrotron Ages, and Frequency-dependent Polarization Attributed to Core-shift
Authors: Minchul Kam, Hiroshi Nagai, Motoki Kino, Keiichi Asada, Rüdiger Kneissl, Iván Agudo, Sascha Trippe, Seiji Kameno, Ioannis Myserlis, Ramprasad Rao, Hojin Cho, Richard A. Perley, Bryan J. Butler, Mark Gurwell, Tomoki Matsuoka, Jongho Park, Carolina Casadio, Baltasar Vila Vilaro, Celia Verdugo, Matias Radiszcz, Kurt Plarre, Wanchaloem Khwammai, Diego Álvarez-Ortega, Juan Escudero, Clemens Thum, Garrett Keating
Figure caption: The blue, magenta, red, and green dots represent the EVPA measurements from ALMA, IRAM, SMA, and VLA, plotted as a function of wavelength squared, respectively. The gray dashed line represents the best fit to the EVPA values.
Paper: Monitoring of 3C 286 with ALMA, IRAM, and SMA from 2006 to 2025: Stability, Synchrotron Ages, and Frequency-dependent Polarization Attributed to Core-shift
Authors: Minchul Kam, Hiroshi Nagai, Motoki Kino, Keiichi Asada, Rüdiger Kneissl, Iván Agudo, Sascha Trippe, Seiji Kameno, Ioannis Myserlis, Ramprasad Rao, Hojin Cho, Richard A. Perley, Bryan J. Butler, Mark Gurwell, Tomoki Matsuoka, Jongho Park, Carolina Casadio, Baltasar Vila Vilaro, Celia Verdugo, Matias Radiszcz, Kurt Plarre, Wanchaloem Khwammai, Diego Álvarez-Ortega, Juan Escudero, Clemens Thum, Garrett Keating
Figure caption: The reference values for the EVPA and fractional polarization of 3C 286 obtained with ALMA, IRAM, SMA (this work), and VLA (R. A. Perley & B. J. Butler 2013b) in the observing frame. Blue, magenta, red, and green colors represent the ALMA, IRAM, SMA, and VLA data, respectively.
Paper: Monitoring of 3C 286 with ALMA, IRAM, and SMA from 2006 to 2025: Stability, Synchrotron Ages, and Frequency-dependent Polarization Attributed to Core-shift
Authors: Minchul Kam, Hiroshi Nagai, Motoki Kino, Keiichi Asada, Rüdiger Kneissl, Iván Agudo, Sascha Trippe, Seiji Kameno, Ioannis Myserlis, Ramprasad Rao, Hojin Cho, Richard A. Perley, Bryan J. Butler, Mark Gurwell, Tomoki Matsuoka, Jongho Park, Carolina Casadio, Baltasar Vila Vilaro, Celia Verdugo, Matias Radiszcz, Kurt Plarre, Wanchaloem Khwammai, Diego Álvarez-Ortega, Juan Escudero, Clemens Thum, Garrett Keating
Figure caption: Top: the total flux of Uranus measured with IRAM at 86 GHz. The blue dashed curve represents the ESA4 model. Bottom: the residual flux, i.e., the excess flux relative to the model normalized by the observed flux, is shown with cross marks. The light blue points represent the average residual flux in bins of 1000 days. The blue dashed line represents the best-fit line to the entire residual flux. The ESA4 model appears to agree best with the data around 2017.
Paper: Self-Consistent Heating of the Magnetically Closed Solar Corona: Generation of Nanoflares, Thermodynamic Response of the Plasma and Observational Signatures
Authors: Craig D. Johnston, Lars K. S. Daldorff, James A. Klimchuk, Shanwlee Sow Mondal, Will T. Barnes, James E. Leake, Jack Reid, Jacob D. Parker
Figure caption: Plasma β (top axis) and temperature (bottom axis) as functions of height for the initial hydrostatic atmosphere. The shaded regions indicate the driving layers that are used to control the imposed photospheric motions.
Paper: Monitoring of 3C 286 with ALMA, IRAM, and SMA from 2006 to 2025: Stability, Synchrotron Ages, and Frequency-dependent Polarization Attributed to Core-shift
Authors: Minchul Kam, Hiroshi Nagai, Motoki Kino, Keiichi Asada, Rüdiger Kneissl, Iván Agudo, Sascha Trippe, Seiji Kameno, Ioannis Myserlis, Ramprasad Rao, Hojin Cho, Richard A. Perley, Bryan J. Butler, Mark Gurwell, Tomoki Matsuoka, Jongho Park, Carolina Casadio, Baltasar Vila Vilaro, Celia Verdugo, Matias Radiszcz, Kurt Plarre, Wanchaloem Khwammai, Diego Álvarez-Ortega, Juan Escudero, Clemens Thum, Garrett Keating
Figure caption: The blue, magenta, red, and green dots represent the fractional polarization measured with ALMA, IRAM, SMA, and VLA, plotted as a function of wavelength squared. The gray dashed line represents the best fit to the fractional polarization values.
Paper: Monitoring of 3C 286 with ALMA, IRAM, and SMA from 2006 to 2025: Stability, Synchrotron Ages, and Frequency-dependent Polarization Attributed to Core-shift
Authors: Minchul Kam, Hiroshi Nagai, Motoki Kino, Keiichi Asada, Rüdiger Kneissl, Iván Agudo, Sascha Trippe, Seiji Kameno, Ioannis Myserlis, Ramprasad Rao, Hojin Cho, Richard A. Perley, Bryan J. Butler, Mark Gurwell, Tomoki Matsuoka, Jongho Park, Carolina Casadio, Baltasar Vila Vilaro, Celia Verdugo, Matias Radiszcz, Kurt Plarre, Wanchaloem Khwammai, Diego Álvarez-Ortega, Juan Escudero, Clemens Thum, Garrett Keating
Figure caption: Total flux of 3C 286 measured with IRAM at 86 GHz and ALMA in Band 3 (top), and with IRAM at 229 GHz and ALMA in Bands 6 and 7 (bottom). Dashed horizontal lines indicate the mean flux values measured with IRAM over its monitoring period for each frequency. Shaded regions correspond to the three periods shown in Figure 2.
Paper: Monitoring of 3C 286 with ALMA, IRAM, and SMA from 2006 to 2025: Stability, Synchrotron Ages, and Frequency-dependent Polarization Attributed to Core-shift
Authors: Minchul Kam, Hiroshi Nagai, Motoki Kino, Keiichi Asada, Rüdiger Kneissl, Iván Agudo, Sascha Trippe, Seiji Kameno, Ioannis Myserlis, Ramprasad Rao, Hojin Cho, Richard A. Perley, Bryan J. Butler, Mark Gurwell, Tomoki Matsuoka, Jongho Park, Carolina Casadio, Baltasar Vila Vilaro, Celia Verdugo, Matias Radiszcz, Kurt Plarre, Wanchaloem Khwammai, Diego Álvarez-Ortega, Juan Escudero, Clemens Thum, Garrett Keating
Figure caption: RM values as a function of geometrical mean frequency for 3C 286 in its rest frame. Each RM value was calculated using the best-fit EVPA values at adjacent VLA and ALMA frequencies, plotted at the geometrical mean frequency of the pairs. The gray dashed line represents the best fit to the RM values.
Paper: Longtime Monitoring of TeV Radio Galaxies with HAWC
Authors: R. Alfaro, C. Alvarez, E. Anita-Rangel, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, P. Bangale, E. Belmont-Moreno, A. Bernal, K. S. Caballero-Mora, T. Capistrán, A. Carramiñana, F. Carreón, S. Casanova, U. Cotti, J. Cotzomi, S. Coutiño de León, E. De la Fuente, D. Depaoli, P. Desiati, N. Di Lalla, R. Diaz Hernandez, M. A. DuVernois, J. C. Díaz-Vélez, K. Engel, T. Ergin, C. Espinoza, N. Fraija, S. Fraija, J. A. García-González, F. Garfias, A. Gonzalez Muñoz, M. M. González, J. A. González, J. A. Goodman, S. Groetsch, J. P. Harding, I. Herzog, D. Huang, F. Hueyotl-Zahuantitla, A. Iriarte, S. Kaufmann, D. Kieda, A. Lara, J. Lee, H. León Vargas, A. L. Longinotti, G. Luis-Raya, K. Malone, O. Martinez, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Morales-Soto, E. Moreno, M. Mostafá, M. Najafi, A. Nayerhoda, L. Nellen, N. Omodei, M. Osorio-Archila, E. Ponce, Y. Pérez Araujo, E. G. Pérez-Pérez, C. D. Rho, A. Rodriguez Parra, D. Rosa-González, M. Roth, H. Salazar, A. Sandoval, M. Schneider, J. Serna-Franco, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, E. Varela, L. Villaseñor, X. Wang, Z. Wang, I. J. Watson, H. Wu, S. Yu, H. Zhou, C. de León
Figure caption: Significance maps obtained with the neural network energy estimator. Top left: M87 is detected with a significance of 5.21σ. Top right: 3C 264 is marginally detected with a significance of 3.99σ. Bottom left: NGC 1275 is not detected, with a maximum significance of 2.21σ at the source position. Bottom right: IC 310 is not detected, with a significance of 1.34σ at the source position. The difference between the bottom maps is the assumed position for the gamma-ray emission search: it is around NGC 1275’s position in the bottom left and around IC 310’s position in the bottom right. The elongated region between NGC 1275 and IC 310, visible in both bottom maps, may suggest a contribution from both sources.
Paper: Self-Consistent Heating of the Magnetically Closed Solar Corona: Generation of Nanoflares, Thermodynamic Response of the Plasma and Observational Signatures
Authors: Craig D. Johnston, Lars K. S. Daldorff, James A. Klimchuk, Shanwlee Sow Mondal, Will T. Barnes, James E. Leake, Jack Reid, Jacob D. Parker
Figure caption: Time-distance plots showing a nanoflare storm and subsequent formation of multithermal clusters in the Z-midplane. The upper three panels show the Jz current density, temperature, and electron number density at y = 16 Mm, and the lower four panels show the emissivities that would be detected in the 171 Å, 193 Å, 94 Å, and 335 Å channels of AIA. The nanoflare storm is indicated by the dashed triangles on the Jz current density and temperature panels, while the cyan boxes on the temperature and 193 Å panels mark the multithermal, multistranded post-storm evolution that is shown close-up in Figure 15. The red arrow indicates the faint signatures of the hot, directly heated plasma in the 94 Å channel.
Paper: Self-Consistent Heating of the Magnetically Closed Solar Corona: Generation of Nanoflares, Thermodynamic Response of the Plasma and Observational Signatures
Authors: Craig D. Johnston, Lars K. S. Daldorff, James A. Klimchuk, Shanwlee Sow Mondal, Will T. Barnes, James E. Leake, Jack Reid, Jacob D. Parker
Figure caption: Close-up of Figure 12 showing the transverse “shifting” of the 193 Å emission, which is caused by phase differences in heating and cooling events across neighboring magnetic flux strands. The green contours show plasma at the peak sensitivity of the 193 Å channel (1.6 MK), while the red (blue) contours indicate hotter (cooler) plasma at 2 MK (1.2 MK). The pink lines on the 193 Å panel mark the “apparent” displacements of the multithermal, multistranded clusters, and the slopes of these lines indicate the speeds associated with these displacements.
Paper: Longtime Monitoring of TeV Radio Galaxies with HAWC
Authors: R. Alfaro, C. Alvarez, E. Anita-Rangel, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, P. Bangale, E. Belmont-Moreno, A. Bernal, K. S. Caballero-Mora, T. Capistrán, A. Carramiñana, F. Carreón, S. Casanova, U. Cotti, J. Cotzomi, S. Coutiño de León, E. De la Fuente, D. Depaoli, P. Desiati, N. Di Lalla, R. Diaz Hernandez, M. A. DuVernois, J. C. Díaz-Vélez, K. Engel, T. Ergin, C. Espinoza, N. Fraija, S. Fraija, J. A. García-González, F. Garfias, A. Gonzalez Muñoz, M. M. González, J. A. González, J. A. Goodman, S. Groetsch, J. P. Harding, I. Herzog, D. Huang, F. Hueyotl-Zahuantitla, A. Iriarte, S. Kaufmann, D. Kieda, A. Lara, J. Lee, H. León Vargas, A. L. Longinotti, G. Luis-Raya, K. Malone, O. Martinez, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Morales-Soto, E. Moreno, M. Mostafá, M. Najafi, A. Nayerhoda, L. Nellen, N. Omodei, M. Osorio-Archila, E. Ponce, Y. Pérez Araujo, E. G. Pérez-Pérez, C. D. Rho, A. Rodriguez Parra, D. Rosa-González, M. Roth, H. Salazar, A. Sandoval, M. Schneider, J. Serna-Franco, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, E. Varela, L. Villaseñor, X. Wang, Z. Wang, I. J. Watson, H. Wu, S. Yu, H. Zhou, C. de León
Figure caption: Left: measured flux (solid black points) and best-fit spectrum (dashed line) of M87. Downward arrows represent upper limits at a 95% confidence level. The fitted spectrum is calculated by assuming an SPL and fixing the pivot energy Ep to 12 TeV. The gray band corresponds to the 1σ error band of the fit. Right: SED of M87 comparing HAWC data (this work) with previous observations from H.E.S.S., VERITAS, and LHAASO at different activity states. HAWC’s measurement is consistent with a low-activity state and represents the longest continuous monitoring of M87 at TeV energies.
Paper: Self-Consistent Heating of the Magnetically Closed Solar Corona: Generation of Nanoflares, Thermodynamic Response of the Plasma and Observational Signatures
Authors: Craig D. Johnston, Lars K. S. Daldorff, James A. Klimchuk, Shanwlee Sow Mondal, Will T. Barnes, James E. Leake, Jack Reid, Jacob D. Parker
Figure caption: EUV emission characteristics of the multithermal clusters. The plot shows the normalized intensity (emission integrated along the LOS as a function of time) in the 171 Å (red), 193 Å (orange), 94 Å (green), and 335 Å (blue) channels of AIA, corresponding to an observation made from the bottom of each emissivity map in Figure 12. The dashed vertical lines correspond to the lifetimes of the 193 Å clusters that were identified in Figure 11 during the same period.
Paper: Self-Consistent Heating of the Magnetically Closed Solar Corona: Generation of Nanoflares, Thermodynamic Response of the Plasma and Observational Signatures
Authors: Craig D. Johnston, Lars K. S. Daldorff, James A. Klimchuk, Shanwlee Sow Mondal, Will T. Barnes, James E. Leake, Jack Reid, Jacob D. Parker
Figure caption: 193 Å light curve for the emissivity averaged over the dashed green box in Figure 9. The dashed vertical lines indicate approximate lifetimes of three different clusters that form during the simulation.
Paper: Self-Consistent Heating of the Magnetically Closed Solar Corona: Generation of Nanoflares, Thermodynamic Response of the Plasma and Observational Signatures
Authors: Craig D. Johnston, Lars K. S. Daldorff, James A. Klimchuk, Shanwlee Sow Mondal, Will T. Barnes, James E. Leake, Jack Reid, Jacob D. Parker
Figure caption: Intensity that would be detected in the 171 Å and 193 Å channels of AIA at t = 440 minutes, for a view from the side that corresponds to a LOS integration along X. The blue boxes mark the point where the intensity is sampled for the light curves plotted in Figure 13, while the dashed blue boxes shows a larger area spanned by the nanoflare storm.