adsabs/AstroCLIMB huggingface dataset:
Paper: Giant Outer Transiting Exoplanet Mass (GOT ‘EM) Survey. IV. Long-term Doppler Spectroscopy for 11 Stars Thought to Host Cool Giant Exoplanets
Authors: Paul A. Dalba, Stephen R. Kane, Howard Isaacson, Benjamin Fulton, Andrew W. Howard, Edward W. Schwieterman, Daniel P. Thorngren, Jonathan Fortney, Noah Vowell, Corey Beard, Sarah Blunt, Casey L. Brinkman, Ashley Chontos, Fei Dai, Steven Giacalone, Michelle L. Hill, Molly Kosiarek, Jack Lubin, Andrew W. Mayo, Teo Močnik, Joseph M. Akana Murphy, Erik A. Petigura, Malena Rice, Ryan A. Rubenzahl, Judah Van Zandt, Lauren M. Weiss, Diana Dragomir, David Kipping, Matthew J. Payne, Arpita Roy, Alex Teachey, Steven Villanueva
Figure caption: Transits and model of the brown dwarf Kepler-807 b folded on the maximum likelihood transit ephemeris. All of the Kepler photometry is long cadence.
Paper: Giant Outer Transiting Exoplanet Mass (GOT ‘EM) Survey. IV. Long-term Doppler Spectroscopy for 11 Stars Thought to Host Cool Giant Exoplanets
Authors: Paul A. Dalba, Stephen R. Kane, Howard Isaacson, Benjamin Fulton, Andrew W. Howard, Edward W. Schwieterman, Daniel P. Thorngren, Jonathan Fortney, Noah Vowell, Corey Beard, Sarah Blunt, Casey L. Brinkman, Ashley Chontos, Fei Dai, Steven Giacalone, Michelle L. Hill, Molly Kosiarek, Jack Lubin, Andrew W. Mayo, Teo Močnik, Joseph M. Akana Murphy, Erik A. Petigura, Malena Rice, Ryan A. Rubenzahl, Judah Van Zandt, Lauren M. Weiss, Diana Dragomir, David Kipping, Matthew J. Payne, Arpita Roy, Alex Teachey, Steven Villanueva
Figure caption: Transits and model of PH-2 b folded on the maximum likelihood transit ephemeris. All of the Kepler photometry is long cadence.
Paper: Giant Outer Transiting Exoplanet Mass (GOT ‘EM) Survey. IV. Long-term Doppler Spectroscopy for 11 Stars Thought to Host Cool Giant Exoplanets
Authors: Paul A. Dalba, Stephen R. Kane, Howard Isaacson, Benjamin Fulton, Andrew W. Howard, Edward W. Schwieterman, Daniel P. Thorngren, Jonathan Fortney, Noah Vowell, Corey Beard, Sarah Blunt, Casey L. Brinkman, Ashley Chontos, Fei Dai, Steven Giacalone, Michelle L. Hill, Molly Kosiarek, Jack Lubin, Andrew W. Mayo, Teo Močnik, Joseph M. Akana Murphy, Erik A. Petigura, Malena Rice, Ryan A. Rubenzahl, Judah Van Zandt, Lauren M. Weiss, Diana Dragomir, David Kipping, Matthew J. Payne, Arpita Roy, Alex Teachey, Steven Villanueva
Figure caption: RVs and best-fit model for Kepler-849.
Paper: Giant Outer Transiting Exoplanet Mass (GOT ‘EM) Survey. IV. Long-term Doppler Spectroscopy for 11 Stars Thought to Host Cool Giant Exoplanets
Authors: Paul A. Dalba, Stephen R. Kane, Howard Isaacson, Benjamin Fulton, Andrew W. Howard, Edward W. Schwieterman, Daniel P. Thorngren, Jonathan Fortney, Noah Vowell, Corey Beard, Sarah Blunt, Casey L. Brinkman, Ashley Chontos, Fei Dai, Steven Giacalone, Michelle L. Hill, Molly Kosiarek, Jack Lubin, Andrew W. Mayo, Teo Močnik, Joseph M. Akana Murphy, Erik A. Petigura, Malena Rice, Ryan A. Rubenzahl, Judah Van Zandt, Lauren M. Weiss, Diana Dragomir, David Kipping, Matthew J. Payne, Arpita Roy, Alex Teachey, Steven Villanueva
Figure caption: RVs and best-fit model for PH-2. The HARPS-N data were adopted from Dubber et al. (2019).
Paper: The Measurement of Masses of OB-type Stars from LAMOST DR5
Authors: Zhenyan Huo, Zhicun Liu, Wenyuan Cui, Chao Liu, Jiaming Liu, Mingxu Sun, Shuai Feng, Linlin Li
Figure caption: Comparison of luminosities (left panel) and masses (right panel) of 100 OB-type stars derived using Gaia DR3 data to the predicted values obtained by using their stellar parameters and the PARSEC model. log(L predicted/L ⊙)) and M predicted/M ⊙ represent the luminosities and masses of OB-type stars obtained using the stellar parameters and PARSEC model, and log(L Mbol/L ⊙)) and M Mbol/M ⊙ represent the luminosities and masses of OB-type stars obtained using the Gaia DR3 data (L Mbol = 4π R 2 σT 4 and g = GM Mbol/R 2). The dashed lines represent the one-to-one correlation.
Paper: The Measurement of Masses of OB-type Stars from LAMOST DR5
Authors: Zhenyan Huo, Zhicun Liu, Wenyuan Cui, Chao Liu, Jiaming Liu, Mingxu Sun, Shuai Feng, Linlin Li
Figure caption: Distribution of 2893 OB-type stars with masses less than 20 M ⊙ in a mass (M) vs. mass relative errors (ΔM/M) diagram. The open blue circles correspond to the B-type stars and the open red circles to the O-type stars. The inset graph shows the distribution of all OB-type stars in this work. In the top and right histograms, the orange, green, and red dashed lines represent 16%, 50%, and 84% , respectively, of the mass (top) and the relative error of mass (right).
Paper: The Measurement of Masses of OB-type Stars from LAMOST DR5
Authors: Zhenyan Huo, Zhicun Liu, Wenyuan Cui, Chao Liu, Jiaming Liu, Mingxu Sun, Shuai Feng, Linlin Li
Figure caption: The histograms show the distribution of 2946 OB-type stars in effective temperature (left panel), surface gravity (middle panel), and metallicity (right panel).
Paper: The Measurement of Masses of OB-type Stars from LAMOST DR5
Authors: Zhenyan Huo, Zhicun Liu, Wenyuan Cui, Chao Liu, Jiaming Liu, Mingxu Sun, Shuai Feng, Linlin Li
Figure caption: Comparison of the masses from the grid point of PARESEC (MassTrue) and the masses estimated using our method (Masspredict); the black dashed line represents the one-to-one relation. The inset graph shows the comparison of masses less than 40 M ⊙.
Paper: The Measurement of Masses of OB-type Stars from LAMOST DR5
Authors: Zhenyan Huo, Zhicun Liu, Wenyuan Cui, Chao Liu, Jiaming Liu, Mingxu Sun, Shuai Feng, Linlin Li
Figure caption: Similar to Figure 3 for the estimated luminosities and relative errors of OB-type stars in this work.
Paper: The Measurement of Masses of OB-type Stars from LAMOST DR5
Authors: Zhenyan Huo, Zhicun Liu, Wenyuan Cui, Chao Liu, Jiaming Liu, Mingxu Sun, Shuai Feng, Linlin Li
Figure caption: Similar to Figure 3 for the estimated radii and relative errors of OB-type stars in this work.
Paper: The Measurement of Masses of OB-type Stars from LAMOST DR5
Authors: Zhenyan Huo, Zhicun Liu, Wenyuan Cui, Chao Liu, Jiaming Liu, Mingxu Sun, Shuai Feng, Linlin Li
Figure caption: Comparison of the mass estimated in this work and those from the literature; the black dashed line represents the one-to-one relation.
Paper: The Measurement of Masses of OB-type Stars from LAMOST DR5
Authors: Zhenyan Huo, Zhicun Liu, Wenyuan Cui, Chao Liu, Jiaming Liu, Mingxu Sun, Shuai Feng, Linlin Li
Figure caption: The distribution of OB-type stars in Galactic longitude vs. Galactic latitude; the color code represents the masses of OB-type stars.
Paper: A Comprehensive Comparison of Various Galactic Cosmic-Ray Models to the State-of-the-art Particle and Radiation Measurements
Authors: Weihao Liu, Jingnan Guo, Yubao Wang, Tony C. Slaba
Figure caption: Comparison of the GCR proton flux between models and measurements: (a) 2010 January, (b) 2014 February, and (c) 2019 October. In each of these three panels, the proton flux given by the DLR, BON20, SDEMMA, HelMod, and CRÈME models is in purple, magenta, yellow, orange, and red, respectively. The measured flux from PAMELA and AMS-02 experiments is plotted as light-green and blue scattered points with systematic errors, respectively. Two additional panels provide the temporal evolution of the comparison: (d) absolute relative difference (﹩\left|{RD}\right|﹩) between the model predictions and measurements and (e) ﹩{\chi }_{\nu }^{2}﹩ value. The light-green shaded area represents the time span when the PAMELA flux data are used (from 2006 July to 2011 April), while the blue shaded area represents the time span when the AMS-02 flux data are used (from 2011 May to 2019 October).
Paper: A Comprehensive Comparison of Various Galactic Cosmic-Ray Models to the State-of-the-art Particle and Radiation Measurements
Authors: Weihao Liu, Jingnan Guo, Yubao Wang, Tony C. Slaba
Figure caption: Comparison of the GCR iron flux between models and measurements: (a) 2010 January, (b) 2014 February, and (c) 2019 October, compared to the ACE/CRIS measurements (deep-blue scattered points), and (d) 8.5 yr averaged iron flux multiplied by E 2.7, compared to the AMS-02 measurements (light-blue scattered points). In each of these four panels, the purple, magenta, yellow, orange, and red curves denote the iron flux of the DLR, BON20, SDEMMA, HelMod, and CRÈME models, respectively. Two additional panels provide the statistical evolution of the flux compared to the ACE/CRIS measurements: (d) absolute relative difference (﹩\left|{RD}\right|﹩) between the model predictions and measurements and (e) ﹩{\chi }_{\nu }^{2}﹩ value.
Paper: A Comprehensive Comparison of Various Galactic Cosmic-Ray Models to the State-of-the-art Particle and Radiation Measurements
Authors: Weihao Liu, Jingnan Guo, Yubao Wang, Tony C. Slaba
Figure caption: Comparison of the GCR argon flux between models and measurements as described in Figure 10, where the measurements are limited to the ACE/CRIS instrument.
Paper: A Comprehensive Comparison of Various Galactic Cosmic-Ray Models to the State-of-the-art Particle and Radiation Measurements
Authors: Weihao Liu, Jingnan Guo, Yubao Wang, Tony C. Slaba
Figure caption: Comparison of the GCR helium flux between models and measurements as described in Figure 8.
Paper: A Comprehensive Comparison of Various Galactic Cosmic-Ray Models to the State-of-the-art Particle and Radiation Measurements
Authors: Weihao Liu, Jingnan Guo, Yubao Wang, Tony C. Slaba
Figure caption: Similar to Figure 6 but for heavy ions with the atomic number (Z) ranging from 3 to 26.
Paper: A Comprehensive Comparison of Various Galactic Cosmic-Ray Models to the State-of-the-art Particle and Radiation Measurements
Authors: Weihao Liu, Jingnan Guo, Yubao Wang, Tony C. Slaba
Figure caption: Comparison of the GCR nitrogen flux between various models and measurements as described in Figure 10.
Paper: A Comprehensive Comparison of Various Galactic Cosmic-Ray Models to the State-of-the-art Particle and Radiation Measurements
Authors: Weihao Liu, Jingnan Guo, Yubao Wang, Tony C. Slaba
Figure caption: Comparison of the GCR carbon flux between various models and measurements as described in Figure 10.
Paper: A Comprehensive Comparison of Various Galactic Cosmic-Ray Models to the State-of-the-art Particle and Radiation Measurements
Authors: Weihao Liu, Jingnan Guo, Yubao Wang, Tony C. Slaba
Figure caption: Comparison of the GCR oxygen flux between various models and measurements as described in Figure 10.
Paper: A Comprehensive Comparison of Various Galactic Cosmic-Ray Models to the State-of-the-art Particle and Radiation Measurements
Authors: Weihao Liu, Jingnan Guo, Yubao Wang, Tony C. Slaba
Figure caption: Comparison of the GCR neon flux between various models and measurements as described in Figure 10.
Paper: The AO327 Drift Survey Catalog and Data Release of Pulsar Detections
Authors: J. S. Deneva, M. McLaughlin, T. E. E. Olszanski, E. F. Lewis, D. Pang, P. C. C. Freire, M. Bagchi, K. Stovall
Figure caption: Black dots show the ratio of flux density S to detection threshold ﹩{S}_{\min }﹩ vs. DM for pulsar detections. Red squares show the same for nondetections where S was estimated using the pulsar spectrum fitting code of Swainston et al. (2022), and red crosses show the ratio for nondetections where S was estimated by a power-law fit to flux density measurements from the ATNF catalog. Section 6 details how S and ﹩{S}_{\min }﹩ were calculated for detections and nondetections. A solid line corresponds to the 6σ detection threshold commonly used in pulsar searches. Our weakest detection is below this threshold as known pulsars can sometimes be visually identified in diagnostic plots even if they would not pass the automated candidate sifting in blind searches, where a lower threshold would result in an overwhelming number of spurious candidates. Green triangles indicate the DMs of nondetections for which W obs > P in Equation (4). In those cases a threshold ﹩{S}_{\min }﹩ cannot be calculated because their pulses are too broadened to be detected regardless of flux density.
Paper: The AO327 Drift Survey Catalog and Data Release of Pulsar Detections
Authors: J. S. Deneva, M. McLaughlin, T. E. E. Olszanski, E. F. Lewis, D. Pang, P. C. C. Freire, M. Bagchi, K. Stovall
Figure caption: Sky coverage of the AO327 survey with the PUPPI spectrometer is shown in gray. Known pulsars from the ATNF catalog are shown as black points. Pulsars included in the AO327 catalog are indicated with blue squares if they were discovered in AO327-PUPPI data by their periodic emisssion and with red circles if they are otherwise known pulsars listed in the ATNF catalog. RRATs and slow pulsars discovered by AO327 via a single-pulse search are not included in the present work if no periodic emission was detected in the AO327 survey data. The concentration of pulsars near R.A. ∼ 18–20h corresponds to the inner Galactic plane.
Paper: The AO327 Drift Survey Catalog and Data Release of Pulsar Detections
Authors: J. S. Deneva, M. McLaughlin, T. E. E. Olszanski, E. F. Lewis, D. Pang, P. C. C. Freire, M. Bagchi, K. Stovall
Figure caption: Phase-aligned NICER (black) and Arecibo 327 MHz (red) pulse profiles of PSR J0751+1807. The radio profiles are in arbitrary units and were normalized to the same peak height as the NICER profiles. The radio pulse profile at the top was made by folding both data sets with the pulsar ephemeris from Guillot et al. (2019). In the bottom panel the NICER data set was folded in the same way, while the AO327 data set was folded using the pulsar DM from the ATNF catalog and the best-fit local P and ﹩\dot{P}﹩ as determined by prepfold. Two full rotations are shown for clarity.
Paper: The AO327 Drift Survey Catalog and Data Release of Pulsar Detections
Authors: J. S. Deneva, M. McLaughlin, T. E. E. Olszanski, E. F. Lewis, D. Pang, P. C. C. Freire, M. Bagchi, K. Stovall
Figure caption: Flux density for pulsar detections at 327 MHz calculated using Equation (3) vs. flux density at 400 MHz from the ATNF catalog. The solid line denotes S 327 = S 400. The three labeled detections are outliers due to nulling (J0302+2252), scintillation (B1534+12), and an apparent outlier S 400 value (J1246+2253). We discuss these points in more detail in Section 5.4.
Paper: The AO327 Drift Survey Catalog and Data Release of Pulsar Detections
Authors: J. S. Deneva, M. McLaughlin, T. E. E. Olszanski, E. F. Lewis, D. Pang, P. C. C. Freire, M. Bagchi, K. Stovall
Figure caption: The gain correction factor (ϵ) vs. δ for several pulsar tracks at different offsets in δ (y) from the beam center, symmetric with respect to the beam axis aligned with the meridian, and with a length equal to the beam diameter (﹩15^{\prime} ﹩).
Paper: Observational Properties of 155 β Cephei Pulsating Variable Stars
Authors: Xiang-dong Shi, Sheng-bang Qian, Li-ying Zhu, Lin-jia Li, Er-gang Zhao, Wen-xu Lin
Figure caption: The H-R diagram of these BCEP stars. The red solid circles represent these BCEP stars and candidates. The BCEP and SPB stars, which were previously published in Papers I and II, are also depicted as red open circles and black solid circles, respectively. Targets with suspected unreliable parameters in Papers I and II were excluded from this diagram. The theoretical zero-age main sequence and evolutionary paths for various masses with Z = 0.02 are represented by the black solid lines. The blue and magenta dotted lines represent the theoretical instability regions of SPB and BCEP stars for Z = 0.02 and spherical harmonic degree l ≤ 3, as documented in Miglio et al. (2007). The black cross in the upper-left corner represents a standard error box.
Paper: Observational Properties of 155 β Cephei Pulsating Variable Stars
Authors: Xiang-dong Shi, Sheng-bang Qian, Li-ying Zhu, Lin-jia Li, Er-gang Zhao, Wen-xu Lin
Figure caption: Distribution of the parameters for BCEP stars.
Paper: Observational Properties of 155 β Cephei Pulsating Variable Stars
Authors: Xiang-dong Shi, Sheng-bang Qian, Li-ying Zhu, Lin-jia Li, Er-gang Zhao, Wen-xu Lin
Figure caption: Example light curves and Fourier spectra for some BCEP stars. The red dotted lines represent the approximate boundary of 3 cycles day−1 for low frequency and high frequency. The Fourier spectra of 83 stars first confirmed as BCEP stars are shown in the Appendix.
Paper: Observational Properties of 155 β Cephei Pulsating Variable Stars
Authors: Xiang-dong Shi, Sheng-bang Qian, Li-ying Zhu, Lin-jia Li, Er-gang Zhao, Wen-xu Lin
Figure caption: The effective temperature and the dominant pulsating-period relation diagram of these BCEP stars. Similar symbols to those in Figure 3 are used, but the size of the circles denotes their pulsation amplitude at the dominant frequency.
Paper: CME Arrival Time Prediction via Fusion of Physical Parameters and Image Features
Authors: Yufeng Zhong, Dong Zhao, Xin Huang, Long Xu
Figure caption: The PFE module is designed for CME physical parameters. The model consists of three linear layers with the ReLU function, as well as an add and normalize layer that constructs the residual connection.
Paper: CME Arrival Time Prediction via Fusion of Physical Parameters and Image Features
Authors: Yufeng Zhong, Dong Zhao, Xin Huang, Long Xu
Figure caption: Our proposed approach comprises three modules: a PFE module, an IFE module, and an FF module. The PFE module extracts features from CME physical parameters and the IFE module extracts features from CME images. The FF module fuses the features of both CME physical parameters and CME images to capture comprehensive and crucial information about CMEs.
Paper: CME Arrival Time Prediction via Fusion of Physical Parameters and Image Features
Authors: Yufeng Zhong, Dong Zhao, Xin Huang, Long Xu
Figure caption: The IFE module employs a ResNet-18 architecture, comprising convolutional layers and pooling layers. The IFE module can automatically extract comprehensive CME-related features from images, including aspects that could be difficult for humans to perceive.
Paper: CME Arrival Time Prediction via Fusion of Physical Parameters and Image Features
Authors: Yufeng Zhong, Dong Zhao, Xin Huang, Long Xu
Figure caption: The visualization of the feature map indicates that the IFE module can automatically extract complete and in-depth CME-related information from images, including features that might be challenging for human perception.
Paper: CME Arrival Time Prediction via Fusion of Physical Parameters and Image Features
Authors: Yufeng Zhong, Dong Zhao, Xin Huang, Long Xu
Figure caption: The comparative study between our method and the Average of all Methods recorded on the CME Scoreboard (https://kauai.ccmc.gsfc.nasa.gov/CMEscoreboard/).
Paper: CME Arrival Time Prediction via Fusion of Physical Parameters and Image Features
Authors: Yufeng Zhong, Dong Zhao, Xin Huang, Long Xu
Figure caption: The attention weight calculated from parameter features and image features can make our model selectively overlook irrelevant image areas and focus solely on regions most crucial to CMEs.
Paper: CME Arrival Time Prediction via Fusion of Physical Parameters and Image Features
Authors: Yufeng Zhong, Dong Zhao, Xin Huang, Long Xu
Figure caption: The visualization of the attention weight. The highlighted area visualizes the weight of different areas in the image, with areas of higher weight closer to red and areas of lower weight closer to blue.
Paper: CME Arrival Time Prediction via Fusion of Physical Parameters and Image Features
Authors: Yufeng Zhong, Dong Zhao, Xin Huang, Long Xu
Figure caption: The comprehensive analysis of our final results. (a) The distribution of AE between calculated and observed transit times for all CME events in the test set. (b) The correlation of predicted and observed transit time of each CME event in the test set.
Paper: Evolution and Final Fate of Solar Metallicity Stars in the Mass Range 7–15 M ⊙. I. The Transition from Asymptotic Giant Branch to Super-AGB Stars, Electron Capture, and Core-collapse Supernova Progenitors
Authors: Marco Limongi, Lorenzo Roberti, Alessandro Chieffi, Ken'ichi Nomoto
Figure caption: Selected properties of a model in which a generic URCA pair  A (N, M) is efficient. Upper left panel: abundance in mass fraction as a function of the interior mass of the two interacting nuclei N and M. Upper right panel: density as a function of the interior mass. Lower left panel: number of captures/decays per unit time in seconds (λ; black lines, right y-axis), number of reactions occurring per unit mass and unit time in grams per second (r; green lines, right y-axis), and nuclear energy of the URCA pair in MeV (E; red lines, right y-axis); the solid lines refer to the EC, while the dashed lines refer to the beta decay. Lower right panel: nuclear energy of the URCA pair in ergs per unit mass and unit time (﹩\varepsilon =-{{rE}}_{\nu }﹩); the black line refers to the EC, the red line to the beta decay, and the orange line to the total of the URCA pair. In all of the panels, the gray vertical dashed line marks the URCA shell.
Paper: Evolution and Final Fate of Solar Metallicity Stars in the Mass Range 7–15 M ⊙. I. The Transition from Asymptotic Giant Branch to Super-AGB Stars, Electron Capture, and Core-collapse Supernova Progenitors
Authors: Marco Limongi, Lorenzo Roberti, Alessandro Chieffi, Ken'ichi Nomoto
Figure caption: Central temperature as a function of the central density during the late stages of models in which the URCA processes are activated.
Paper: Evolution and Final Fate of Solar Metallicity Stars in the Mass Range 7–15 M ⊙. I. The Transition from Asymptotic Giant Branch to Super-AGB Stars, Electron Capture, and Core-collapse Supernova Progenitors
Authors: Marco Limongi, Lorenzo Roberti, Alessandro Chieffi, Ken'ichi Nomoto
Figure caption: Convective (green shaded areas) and chemical (color codes reported in the color bar) internal history of the 9 M ⊙ model during the late phase of the second dredge-up. The x-axis reports the logarithm of the time until the end of the evolution (t fin − t) in units of years.
Paper: Evolution and Final Fate of Solar Metallicity Stars in the Mass Range 7–15 M ⊙. I. The Transition from Asymptotic Giant Branch to Super-AGB Stars, Electron Capture, and Core-collapse Supernova Progenitors
Authors: Marco Limongi, Lorenzo Roberti, Alessandro Chieffi, Ken'ichi Nomoto
Figure caption: Temperature gradients (see the legend) as a function of the interior mass of the 9.2 M ⊙ star at selected times during the formation of the convective core associated with the 25(Mg, Na) URCA pair, marked by the values of the central densities in units of g cm−3. According to the adopted stability criterion (see text), convection sets in when the radiative gradient becomes larger than the adiabatic one. Let us remember that the actual temperature gradient used is the adiabatic one in the convective zones and the radiative one in the radiative layers.
Paper: Evolution and Final Fate of Solar Metallicity Stars in the Mass Range 7–15 M ⊙. I. The Transition from Asymptotic Giant Branch to Super-AGB Stars, Electron Capture, and Core-collapse Supernova Progenitors
Authors: Marco Limongi, Lorenzo Roberti, Alessandro Chieffi, Ken'ichi Nomoto
Figure caption: Same as Figure 20 but during a phase in which a convective core, driven by the 23(Na, Ne) URCA pair, and a convective shell, induced by the 25(Mg, Na) URCA pair, are formed. The gray and green vertical dashed lines mark the 25(Mg, Na) and 23(Na, Ne) URCA shells, respectively.
Paper: Evolution and Final Fate of Solar Metallicity Stars in the Mass Range 7–15 M ⊙. I. The Transition from Asymptotic Giant Branch to Super-AGB Stars, Electron Capture, and Core-collapse Supernova Progenitors
Authors: Marco Limongi, Lorenzo Roberti, Alessandro Chieffi, Ken'ichi Nomoto
Figure caption: Selected quantities of the 9.20 M ⊙ model during the breathing pulses induced by the 23(Na, Ne) URCA pair: the central 23Na mass fraction (green line, left y-axis), the mass of the convective core (blue line, right y-axis), and the central temperature (red line, right y-axis).