adsabs/AstroCLIMB huggingface dataset:
Paper: Unprecedented Early Flux Excess in the Hybrid 02es-like Type Ia Supernova 2022ywc Indicates Interaction with Circumstellar Material
Authors: Shubham Srivastav, T. Moore, M. Nicholl, M. R. Magee, S. J. Smartt, M. D. Fulton, S. A. Sim, J. M. Pollin, L. Galbany, C. Inserra, A. Kozyreva, Takashi J. Moriya, F. P. Callan, X. Sheng, K. W. Smith, J. S. Sommer, J. P. Anderson, M. Deckers, M. Gromadzki, T. E. Müller-Bravo, G. Pignata, A. Rest, D. R. Young
Figure caption: ATLAS light curve of SN 2022ywc along with draws from the posterior of the CSMNI model from MOSFiT. The c-band light curve and model are shifted for clarity. The explosion epoch, which is one of the free parameters in the model, is MJD ﹩{59875.1}_{-0.7}^{+0.6}﹩.
Paper: Unprecedented Early Flux Excess in the Hybrid 02es-like Type Ia Supernova 2022ywc Indicates Interaction with Circumstellar Material
Authors: Shubham Srivastav, T. Moore, M. Nicholl, M. R. Magee, S. J. Smartt, M. D. Fulton, S. A. Sim, J. M. Pollin, L. Galbany, C. Inserra, A. Kozyreva, Takashi J. Moriya, F. P. Callan, X. Sheng, K. W. Smith, J. S. Sommer, J. P. Anderson, M. Deckers, M. Gromadzki, T. E. Müller-Bravo, G. Pignata, A. Rest, D. R. Young
Figure caption: 2D posteriors for the main physical parameters in the MOSFiT CSMNI model fit to SN 2022ywc. R 0 is in units of 1014 cm, and ﹩{t}_{\exp }﹩ is relative to MJD 59878.02.
Paper: Electromagnetic Precursors to Black Hole–Neutron Star Gravitational Wave Events: Flares and Reconnection-powered Fast Radio Transients from the Late Inspiral
Authors: Elias R. Most, Alexander A. Philippov
Figure caption: EM luminosities, ﹩{{ \mathcal L }}_{\mathrm{EM}}﹩, for GW200115-like models for various inclination angles, θ NS, of the NS’s magnetic field. Normalizations are given relative to the moving dipole estimate, ﹩{{ \mathcal L }}_{\mathrm{dipole}}﹩, see also Equation (1), as well as to the orbital period, t orbit. All luminosities have been computed at a distance r = 500 km from the system.
Paper: The Effect of Irradiation on the Spin of Millisecond Pulsars
Authors: Shun-Yi Lan, Xiang-Cun Meng
Figure caption: Evolution tracks of radio phases in the ﹩{P}_{\mathrm{spin}}\mbox{--}{\dot{P}}_{\mathrm{spin}}﹩ diagram, corresponding to Figure 1. The blue solid and red dashed lines indicate η = 0 and 0.1, respectively. All line segments indicate r mag > r lc. The initial values of magnetic fields for both evolutions are μ 0 = 4.0 × 1031 G cm3. Solid circles and triangles are the evolution start and end points, respectively. The green solid star presents the PSR J1402+13. The black points are the current pulsar population, and data are from https://www.atnf.csiro.au/research/pulsar/psrcat/.
Paper: The Effect of Irradiation on the Spin of Millisecond Pulsars
Authors: Shun-Yi Lan, Xiang-Cun Meng
Figure caption: Evolution of mass transfer rate value. The initial mass of the companion star is M 2 = 1.0 M ⊙ and initial orbital period is P orb = 5.0 days. Irradiation efficiencies are η = 0 (top) and η = 0.1 (bottom).
Paper: The Effect of Irradiation on the Spin of Millisecond Pulsars
Authors: Shun-Yi Lan, Xiang-Cun Meng
Figure caption: Evolution of spin period corresponding to Figure 1. Blue solid and red dashed lines indicate irradiation efficiencies η = 0 and 0.1, respectively. The initial values of magnetic fields for both evolutions are μ 0 = 4.0 × 1031 G cm3.
Paper: The Effect of Irradiation on the Spin of Millisecond Pulsars
Authors: Shun-Yi Lan, Xiang-Cun Meng
Figure caption: Evolution of the mass of NS corresponding to Figure 1. Blue solid and green dashed lines indicate irradiation efficiencies η = 0 and 0.1, respectively.
Paper: Electromagnetic Precursors to Black Hole–Neutron Star Gravitational Wave Events: Flares and Reconnection-powered Fast Radio Transients from the Late Inspiral
Authors: Elias R. Most, Alexander A. Philippov
Figure caption: Three-dimensional magnetic field line visualization of a flaring event for a GW200115-like binary with a magnetic dipole with θ NS = 60° inclination. Shown are selected field line bundles for three different times, t, relative to the orbital period, t orbit. Left: closed magnetic field lines get initially accreted and pinned onto the BH. Center: continued orbital motion begins twisting the connected field lines, inflating the connected flux tube. Right: the flare detaches from the binary as can be seen by field lines disconnecting from the BH (due to reconnection in the trailing current sheet). The strong twist is visible as a toroidal component of the inflated flux tube. Colors indicate logarithmic magnetic field strengths in relative units.
Paper: Electromagnetic Precursors to Black Hole–Neutron Star Gravitational Wave Events: Flares and Reconnection-powered Fast Radio Transients from the Late Inspiral
Authors: Elias R. Most, Alexander A. Philippov
Figure caption: Interaction of a BH (right) with the magnetic field lines of an NS (left) shortly before merger.
Paper: Unprecedented Early Flux Excess in the Hybrid 02es-like Type Ia Supernova 2022ywc Indicates Interaction with Circumstellar Material
Authors: Shubham Srivastav, T. Moore, M. Nicholl, M. R. Magee, S. J. Smartt, M. D. Fulton, S. A. Sim, J. M. Pollin, L. Galbany, C. Inserra, A. Kozyreva, Takashi J. Moriya, F. P. Callan, X. Sheng, K. W. Smith, J. S. Sommer, J. P. Anderson, M. Deckers, M. Gromadzki, T. E. Müller-Bravo, G. Pignata, A. Rest, D. R. Young
Figure caption: Spectral evolution of SN 2022ywc between +3d and +58d relative to maximum. Also plotted for comparison are the spectra of the hybrid 02es-like Ia SN 2006bt (Foley et al. 2010), SN 2007cq (Ganeshalingam et al. 2010), and SN 2016jhr (Jiang et al. 2017), the 91bg-like SN 1999by (Matheson et al. 2008) and the normal Ia SN 2011fe (Mazzali et al. 2014; Zhang et al. 2016) at similar phases. Top panel shows the +3d spectrum of SN 2022ywc compared to three double detonation models of Polin et al. (2019), computed for a WD mass of 1.0 M ⊙ and He shell masses of 0.01, 0.03, and 0.05 M ⊙. The model spectra were shifted along y-axis for clarity, but not scaled in wavelength or flux axes relative to the observed spectrum. Prominent telluric features are marked with the symbol ⊕. The ATLAS orange and cyan filter response curves are also shown for reference.
Paper: Ice Sublimation in Planetesimals Formed at the Outward Migrating Snowline
Authors: Zhongtian Zhang
Figure caption: The maximum pore (gas) pressure inside a 100 km radius planetesimal. The curves of different colors are results at different micropore sizes and thus different micropermeabilities. The solid curves show the general solution, Equation (14); the dotted curves are asymptotic solutions, Equations (15) and (16). The horizontal line shows the water triple point pressure (6 mbar).
Paper: Unprecedented Early Flux Excess in the Hybrid 02es-like Type Ia Supernova 2022ywc Indicates Interaction with Circumstellar Material
Authors: Shubham Srivastav, T. Moore, M. Nicholl, M. R. Magee, S. J. Smartt, M. D. Fulton, S. A. Sim, J. M. Pollin, L. Galbany, C. Inserra, A. Kozyreva, Takashi J. Moriya, F. P. Callan, X. Sheng, K. W. Smith, J. S. Sommer, J. P. Anderson, M. Deckers, M. Gromadzki, T. E. Müller-Bravo, G. Pignata, A. Rest, D. R. Young
Figure caption: Predicted peak luminosity vs. luminosity for the bump or early excess in the double detonation models of Magee et al. (2021) computed for o band. The colors represent the WD masses, and symbols represent the He shell mass. The shaded region highlights the models with a peak luminosity that is consistent with that of SN 2022ywc. The peak magnitude of SN 2022ywc and the associated uncertainty were estimated using the method described in Section 3.2.
Paper: Ice Sublimation in Planetesimals Formed at the Outward Migrating Snowline
Authors: Zhongtian Zhang
Figure caption: Cartoon illustrations of different spatial scales of a planetesimal (a) formed through “streaming instabilities” by up to meter-sized boulders (b), which themselves are aggregates of submicrometer dust grains (c). The planetesimal is inside the outward-migrating snowline, and water vapor can be lost to the surrounding nebula from its surface (panel (a)). Inside the planetesimal, vapor is transported along the macropores between boulders (panel (b)). Inside the boulders, vapor is generated and transported along the micropores (panel (c)) toward the macropores.
Paper: Outlier Detection in the DESI Bright Galaxy Survey
Authors: Yan Liang, Peter Melchior, ChangHoon Hahn, Jeff Shen, Andy Goulding, Charlotte Ward
Figure caption: DESI MWS spectra (black) and their reconstructed models (red) from our star AE. Panels as in Figure 2.
Paper: Outlier Detection in the DESI Bright Galaxy Survey
Authors: Yan Liang, Peter Melchior, ChangHoon Hahn, Jeff Shen, Andy Goulding, Charlotte Ward
Figure caption: Representative selection of outliers in BGS identified by the galaxy AE and normalizing flow, in decreasing order of the outlier score (details for each object in Section 4). The panels are identical to Figure 2, but for visual clarity, we omitted showing the AE model. The legend in the upper left corner includes the DESI Target ID, Redrock redshift, reduced chi-square of the AE model, and the negative log probability of the NF model. The red dashed lines in the bottom panel indicate prominent features of a suspected broad absorption line quasar at z = 1.53.
Paper: Outlier Detection in the DESI Bright Galaxy Survey
Authors: Yan Liang, Peter Melchior, ChangHoon Hahn, Jeff Shen, Andy Goulding, Charlotte Ward
Figure caption: BGS galaxy spectra (black) and their reconstructed models (red) as determined by our spectrum AE. The main panels present the entire flux-normalized restframe spectrum, assuming the Redrock redshift, with regions masked during training shaded in gray. The upper left panels provide zoomed-in views of significant emission/absorption lines, while the upper right panels show the image of the source from the DESI Legacy Imaging Surveys with the fiber size indicated in red.
Paper: Outlier Detection in the DESI Bright Galaxy Survey
Authors: Yan Liang, Peter Melchior, ChangHoon Hahn, Jeff Shen, Andy Goulding, Charlotte Ward
Figure caption: Our approach combines an AE for spectrum reconstruction and an NF for probability estimation. The AE compresses an observed galaxy spectrum into a low-dimensional latent representation of the restframe spectrum, and the NF transforms the latent distribution of the entire BGS galaxy sample into a Gaussian base distribution for efficient probability computation and sampling.
Paper: Outlier Detection in the DESI Bright Galaxy Survey
Authors: Yan Liang, Peter Melchior, ChangHoon Hahn, Jeff Shen, Andy Goulding, Charlotte Ward
Figure caption: Comparison of observed spectra (black) and model fits (Redrock galaxy model (cyan), Redrock star model (blue), and our star AE model (red)) for two example stars misclassified as galaxies by Redrock. Shaded regions indicate areas masked due to telluric contamination.
Paper: The Transient Outgassed Atmosphere of 55 Cancri e
Authors: Kevin Heng
Figure caption: Schematic of multiwavelength model that includes a hot rocky surface (heated by starlight) and a thin, transient atmosphere sourced by geochemical outgassing. The left and right panels show the model in its “bare rock” and thin-atmosphere phases, respectively. The atmosphere is transient because outgassing and atmospheric escape fail to balance out each other and the timescale for adjustment to radiative equilibrium is likely to be shorter than an orbital period (see the text for discussion).
Paper: The Transient Outgassed Atmosphere of 55 Cancri e
Authors: Kevin Heng
Figure caption: Emission spectra (wavelength-dependent secondary eclipse depths) for P = 0.1 bar, T = 2700 K, and T  s  = 1965 K. The gray dotted curves represent “bare rock” models with various assumed values for the geometric albedo of the rocky surface (A  g,s ). The A  g,s  = 0 curve essentially corresponds to a 1965 K blackbody. For Rayleigh scattering, A  g  = 0.77 when ω = 1. The black dashed curve corresponds to a 2700 K blackbody.
Paper: The Transient Outgassed Atmosphere of 55 Cancri e
Authors: Kevin Heng
Figure caption: Scattering photospheric pressures (top left panel), single-scattering albedos (top right panel), absorption cross sections (bottom left panel), and absorption photospheric pressures (bottom right panel) associated with pure carbon dioxide (CO2), carbon monoxide (CO), and methane (CH4) atmospheres. For the absorption cross sections, a temperature of 2700 K and a pressure of 0.1 bar are assumed.
Paper: The Transient Outgassed Atmosphere of 55 Cancri e
Authors: Kevin Heng
Figure caption: The same as Figure 3, but for P = 1 mbar. Since this atmosphere is optically thin to Rayleigh scattering, the treatment of multiple scattering is ignored; see Equation (8).
Paper: Varstrometry for Off-nucleus and Dual Subkiloparsec AGN (VODKA). SDSS J1608+2716: A Subarcsecond Quadruply Lensed Quasar at z = 2.575
Authors: Junyao Li, Xin Liu, Yue Shen, Masamune Oguri, Arran C. Gross, Nadia L. Zakamska, Yu-Ching Chen, Hsiang-Chih Hwang
Figure caption: Quasar-galaxy decomposition result using a four PSF (for A, B, C, and D) + two Sérsic (for G1 and G2) model: (a) observed image with a logarithm scaling; (b) best-fit model image convolved with the PSF; (c) data minus the four PSFs (i.e., the pure galaxy image); (d) fitting residuals (model—data) divided by the error map. The black curve marks the warped disk of G1.
Paper: High-resolution Spectroscopic Metallicities of Milky Way Cepheid Standards and Their Impact on the Leavitt Law and the Hubble Constant
Authors: Anupam Bhardwaj, Adam G. Riess, Giovanni Catanzaro, Erasmo Trentin, Vincenzo Ripepi, Marina Rejkuba, Marcella Marconi, Chow-Choong Ngeow, Lucas M. Macri, Martino Romaniello, Roberto Molinaro, Harinder P. Singh, Shashi M. Kanbur
Figure caption: Histograms of metallicities (in gray) for Cepheids from Genovali et al. (2015) that were used in Riess et al. (2021). Our homogenized sample of [Fe/H]ESP values (in pink) for all 75 Cepheids are also overplotted. The solid and dashed lines represent the Gaussian fits to our [Fe/H] values and those from Genovali et al. (2015), respectively. “M” is the mean value of metallicity for the sample of N stars.
Paper: High-resolution Spectroscopic Metallicities of Milky Way Cepheid Standards and Their Impact on the Leavitt Law and the Hubble Constant
Authors: Anupam Bhardwaj, Adam G. Riess, Giovanni Catanzaro, Erasmo Trentin, Vincenzo Ripepi, Marina Rejkuba, Marcella Marconi, Chow-Choong Ngeow, Lucas M. Macri, Martino Romaniello, Roberto Molinaro, Harinder P. Singh, Shashi M. Kanbur
Figure caption: Comparison of our [Fe/H]ESP values with measurements from Luck (L18, 2018), Genovali et al. (G15, 2015), Ngeow (N12, 2012), and Acharova et al. (A12, 2012). The mean offsets, standard deviation, and the number of common stars are listed on the bottom right of each panel. The dashed and dotted lines represent the mean and ±2.5σ offsets, respectively.
Paper: High-resolution Spectroscopic Metallicities of Milky Way Cepheid Standards and Their Impact on the Leavitt Law and the Hubble Constant
Authors: Anupam Bhardwaj, Adam G. Riess, Giovanni Catanzaro, Erasmo Trentin, Vincenzo Ripepi, Marina Rejkuba, Marcella Marconi, Chow-Choong Ngeow, Lucas M. Macri, Martino Romaniello, Roberto Molinaro, Harinder P. Singh, Shashi M. Kanbur
Figure caption: Period–luminosity–metallicity (left) and period–Wesenheit–metallicity (right) relations for 68 MW Cepheids at multiple bands. The dashed lines represent the best-fitting linear regression.
Paper: Early Time Spectropolarimetry of the Aspherical Type II Supernova SN 2023ixf
Authors: Sergiy S. Vasylyev, Yi Yang, 轶 杨, Alexei V. Filippenko, Kishore C. Patra, Thomas G. Brink, Lifan Wang, Ryan Chornock, Raffaella Margutti, Elinor L. Gates, Adam J. Burgasser, Preethi R. Karpoor, Natalie LeBaron, Emma Softich, Christopher A. Theissen, Eli Wiston, WeiKang Zheng
Figure caption: Spectropolarimetry of SN 2023ixf on day +1.4 (epoch 1) relative to an estimated time of first light on MJD 60,082.83. The five panels (from top to bottom) present (a) the arbitrarily scaled flux density, f  λ  (black line), and the polarized flux densities as indicated by the quantities ∣q∣ × f  λ  (navy histogram) and ∣u∣ × f  λ  (orange histogram). Major spectral features at zero velocity are labeled and marked by vertical gray lines; (b, c) the fractional Stokes parameters q and u, respectively; (d) p%; and (e) the polarization PA. In panels (b)–(e), the data have been rebinned to 30 Å for clarity. No ISP correction has been applied. Light-blue shaded vertical bands mark the regions of major telluric absorptions (which have been almost entirely removed through comparisons with standard-star spectra). The light shaded histogram in each panel indicates the 1σ uncertainties.(The data used to create this figure are available.)
Paper: Early Time Spectropolarimetry of the Aspherical Type II Supernova SN 2023ixf
Authors: Sergiy S. Vasylyev, Yi Yang, 轶 杨, Alexei V. Filippenko, Kishore C. Patra, Thomas G. Brink, Lifan Wang, Ryan Chornock, Raffaella Margutti, Elinor L. Gates, Adam J. Burgasser, Preethi R. Karpoor, Natalie LeBaron, Emma Softich, Christopher A. Theissen, Eli Wiston, WeiKang Zheng
Figure caption: Temporal evolution of the continuum polarization of SN 2023ixf from days +2 to +15 after the explosion displayed in the Stokes q−u plane. The continuum is calculated over the wavelength range 5600–6400 Å. The phases of the measurements are relative to an estimated time of first light of MJD 60,082.75 (Hosseinzadeh et al. 2023; Smith et al. 2023). The scale of the lower-left cross represents the typical systematic error as estimated from adopting various parameters during the extraction of the individual spectrum obtained during the polarization measurement. The outer and the inner solid circles mark the 1.0% and the 0.5% contours of the polarization level, respectively. The dashed blue circle indicates the upper limit on the ISP, p ISP ≲ 0.35%.(The data used to create this figure are available.)
Paper: Early Time Spectropolarimetry of the Aspherical Type II Supernova SN 2023ixf
Authors: Sergiy S. Vasylyev, Yi Yang, 轶 杨, Alexei V. Filippenko, Kishore C. Patra, Thomas G. Brink, Lifan Wang, Ryan Chornock, Raffaella Margutti, Elinor L. Gates, Adam J. Burgasser, Preethi R. Karpoor, Natalie LeBaron, Emma Softich, Christopher A. Theissen, Eli Wiston, WeiKang Zheng
Figure caption: Temporal evolution of the polarization spectrum of SN 2023ixf from days +1.4 to +4.6 as shown from the top to bottom panels. In each panel, p and PA are shown by the magenta and green histograms, respectively. The gray line presents the arbitrarily scaled flux-density spectrum. At days +1.4 and +2.5, the “flash” features (FWHM ≈1000 km s−1) display PA ≈ 160° that is consistent with the continuum. At day +3.5, the continuum polarization has decreased from ∼1.0% to ∼0.5%. He II λ4686 and the Balmer lines are broadened (FWHM ≈1000 km s−1). The PA over the emission lines also exhibits a progressive modulation toward ∼220° toward the inner wings. After the CSM that produces the “flash” features has been swept away by the expanding ejecta at day +4.6, the continuum polarization has settled to a level of 0.5% and PA ≈ 220° after a further rotation in the Stokes q−u plane compared to day +3.5 (see Figure 3). The rapidly evolving polarization across the continuum, the Balmer lines, and He II λ4686 during the disappearance of the “flash” features implies that aspherical ejecta break out through an aspherical CSM within the first 5 days after the SN explosion.(The data used to create this figure are available.)
Paper: Early Time Spectropolarimetry of the Aspherical Type II Supernova SN 2023ixf
Authors: Sergiy S. Vasylyev, Yi Yang, 轶 杨, Alexei V. Filippenko, Kishore C. Patra, Thomas G. Brink, Lifan Wang, Ryan Chornock, Raffaella Margutti, Elinor L. Gates, Adam J. Burgasser, Preethi R. Karpoor, Natalie LeBaron, Emma Softich, Christopher A. Theissen, Eli Wiston, WeiKang Zheng
Figure caption: A simplified schematic sketch of the temporal evolution of the ejecta and CSM geometry of SN 2023ixf as inferred from spectropolarimetry, viewed from a direction perpendicular to the plane of the sky. Arbitrary scales and the axis ratios of the ejecta and the CSM are used for illustration purposes. The actual axis ratio that effectively characterizes the degree of asphericity of the CSM depends on its radial density profile, electron-scattering optical depth, and viewing angle. Left: configuration ≲ +2.5 days, when the SN ejecta are still enclosed within the outer bound of the dense, aspherical CSM. The photosphere is in a breakout region within the CSM that is enriched by preexplosion mass loss from the progenitor; the continuum and the short-lived, narrow, highly ionized features are from the CSM. Middle: the transitional phase between days +2.5 and +4.6 when the aspherical SN ejecta emerge from the CSM. Right: the expanding ejecta engulf the CSM, as indicated by the disappearance of the shock-ionized “flash” features. The SN ejecta take over the CSM as the main optical emission source after day +4.6.
Paper: Early Time Spectropolarimetry of the Aspherical Type II Supernova SN 2023ixf
Authors: Sergiy S. Vasylyev, Yi Yang, 轶 杨, Alexei V. Filippenko, Kishore C. Patra, Thomas G. Brink, Lifan Wang, Ryan Chornock, Raffaella Margutti, Elinor L. Gates, Adam J. Burgasser, Preethi R. Karpoor, Natalie LeBaron, Emma Softich, Christopher A. Theissen, Eli Wiston, WeiKang Zheng
Figure caption: Same as Figure 1, but for day +2.5 (epoch 2).(The data used to create this figure are available.)
Paper: Early Time Spectropolarimetry of the Aspherical Type II Supernova SN 2023ixf
Authors: Sergiy S. Vasylyev, Yi Yang, 轶 杨, Alexei V. Filippenko, Kishore C. Patra, Thomas G. Brink, Lifan Wang, Ryan Chornock, Raffaella Margutti, Elinor L. Gates, Adam J. Burgasser, Preethi R. Karpoor, Natalie LeBaron, Emma Softich, Christopher A. Theissen, Eli Wiston, WeiKang Zheng
Figure caption: Same as Figure 1, but for day +3.5 (epoch 3).(The data used to create this figure are available.)
Paper: Estimates of Proton and Electron Heating Rates Extended to the Near-Sun Environment
Authors: R. Bandyopadhyay, C. M. Meyer, W. H. Matthaeus, D. J. McComas, S. R. Cranmer, J. S. Halekas, J. Huang, D. E. Larson, R. Livi, A. Rahmati, P. L. Whittlesey, M. L. Stevens, J. C. Kasper, S. D. Bale
Figure caption: In situ measurements for the fast solar wind: (a) plasma temperature, (b) electron heat conduction flux, and (c) electron density. Binned PSP (dots), Helios (squares), and Ulysses (triangles) data are shown in all plots, with protons in red and electrons in blue. Whenever binning has been performed, we have plotted the original data points in smaller, translucent symbols.
Paper: Estimates of Proton and Electron Heating Rates Extended to the Near-Sun Environment
Authors: R. Bandyopadhyay, C. M. Meyer, W. H. Matthaeus, D. J. McComas, S. R. Cranmer, J. S. Halekas, J. Huang, D. E. Larson, R. Livi, A. Rahmati, P. L. Whittlesey, M. L. Stevens, J. C. Kasper, S. D. Bale
Figure caption: Proton-heating-to-total-heating ratio vs. heliocentric distance. Uncertainty envelopes are described in text.
Paper: Estimates of Proton and Electron Heating Rates Extended to the Near-Sun Environment
Authors: R. Bandyopadhyay, C. M. Meyer, W. H. Matthaeus, D. J. McComas, S. R. Cranmer, J. S. Halekas, J. Huang, D. E. Larson, R. Livi, A. Rahmati, P. L. Whittlesey, M. L. Stevens, J. C. Kasper, S. D. Bale
Figure caption: Empirically derived heating rates vs. heliocentric distance. Also shown are the error envelopes described in the text.
Paper: Estimates of Proton and Electron Heating Rates Extended to the Near-Sun Environment
Authors: R. Bandyopadhyay, C. M. Meyer, W. H. Matthaeus, D. J. McComas, S. R. Cranmer, J. S. Halekas, J. Huang, D. E. Larson, R. Livi, A. Rahmati, P. L. Whittlesey, M. L. Stevens, J. C. Kasper, S. D. Bale
Figure caption: Total heating rates (proton plus electron) vs. heliocentric distance. Error envelopes are described in text. The purple stars are the heating rate estimated using MHD cascade by Bandyopadhyay et al. (2020a).