adsabs/AstroCLIMB huggingface dataset:
Paper: First Results from the JWST Early Release Science Program Q3D: Benchmark Comparison of Optical and Mid-infrared Tracers of a Dusty, Ionized Red Quasar Wind at z = 0.435
Authors: David S. N. Rupke, Dominika Wylezalek, Nadia L. Zakamska, Sylvain Veilleux, Caroline Bertemes, Yuzo Ishikawa, Weizhe Liu, Swetha Sankar, Andrey Vayner, Hui Xian Grace Lim, Ryan McCrory, Grey Murphree, Lillian Whitesell, Lu Shen, Guilin Liu, Jorge K. Barrera-Ballesteros, Hsiao-Wen Chen, Nadiia Diachenko, Andy D. Goulding, Jenny E. Greene, Kevin N. Hainline, Fred Hamann, Timothy Heckman, Sean D. Johnson, Dieter Lutz, Nora Lützgendorf, Vincenzo Mainieri, Nicole P. H. Nesvadba, Patrick Ogle, Eckhard Sturm
Figure caption: Map of [O III]/[S IV] and A V, estimated from a model in which the intrinsic line ratio is near the maximum observed (∼16) and smaller values are due to differential obscuration. The redshifted, receding side of the outflow is preferentially extincted due to obscuration by, e.g., the host galaxy. Extinctions are calculated using Chiar & Tielens (2006).
Paper: First Glycine Isomer Detected in the Interstellar Medium: Glycolamide (NH2C(O)CH2OH)
Authors: Víctor M. Rivilla, Miguel Sanz-Novo, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Laura Colzi, Shaoshan Zeng, Andrés Megías, Álvaro López-Gallifa, Antonio Martínez-Henares, Sarah Massalkhi, Belén Tercero, Pablo de Vicente, Sergio Martín, David San Andrés, Miguel A. Requena-Torres, José Luis Alonso
Figure caption: Unblended or slightly blended transitions of glycolamide detected toward the G+0.693, displayed in order of decreasing line intensity. The observed spectrum is shown as a gray histogram. The best LTE fit derived with MADCUBA for the syn-glycolamide emission is shown with a red curve. The blue curve represents the total modeled emission considering all of the species identified toward this molecular cloud. In the center, the molecular structure of the syn conformer of glycolamide is shown. Carbon atoms are in gray, oxygen atoms in red, nitrogen atoms in blue, and hydrogen atoms in white.
Paper: First Glycine Isomer Detected in the Interstellar Medium: Glycolamide (NH2C(O)CH2OH)
Authors: Víctor M. Rivilla, Miguel Sanz-Novo, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Laura Colzi, Shaoshan Zeng, Andrés Megías, Álvaro López-Gallifa, Antonio Martínez-Henares, Sarah Massalkhi, Belén Tercero, Pablo de Vicente, Sergio Martín, David San Andrés, Miguel A. Requena-Torres, José Luis Alonso
Figure caption: Molecular abundances with respect to H2 of C2H5O2N isomers as a function of relative energy (see Table 1). The red dot corresponds to the detection of syn-glycolamide, while the blue triangles indicate the upper limits derived for the other isomers. The solid red line indicates the expected molecular abundance of the C2H5O2N isomeric family assuming the thermodynamic population at T k = 100 K and using the abundance of syn-glycolamide as a reference.
Paper: First Glycine Isomer Detected in the Interstellar Medium: Glycolamide (NH2C(O)CH2OH)
Authors: Víctor M. Rivilla, Miguel Sanz-Novo, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Laura Colzi, Shaoshan Zeng, Andrés Megías, Álvaro López-Gallifa, Antonio Martínez-Henares, Sarah Massalkhi, Belén Tercero, Pablo de Vicente, Sergio Martín, David San Andrés, Miguel A. Requena-Torres, José Luis Alonso
Figure caption: Proposed chemical network for the formation of glycolamide in the ISM. The red left panel includes oxygen-bearing species, while the blue right panel includes nitrogen- and oxygen-bearing species. Closed-shell species are labeled in bold, as opposed to radicals.
Paper: First Glycine Isomer Detected in the Interstellar Medium: Glycolamide (NH2C(O)CH2OH)
Authors: Víctor M. Rivilla, Miguel Sanz-Novo, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Laura Colzi, Shaoshan Zeng, Andrés Megías, Álvaro López-Gallifa, Antonio Martínez-Henares, Sarah Massalkhi, Belén Tercero, Pablo de Vicente, Sergio Martín, David San Andrés, Miguel A. Requena-Torres, José Luis Alonso
Figure caption: Comparison of the relative molecular abundances, compared to acetamide, of the proposed precursors of glycolamide, derived toward G+0.693 (purple) and the hot cores Sgr B2(N2) (yellow) and G31 (green). The upper limits of glycolamide are indicated with arrows.
Paper: First Glycine Isomer Detected in the Interstellar Medium: Glycolamide (NH2C(O)CH2OH)
Authors: Víctor M. Rivilla, Miguel Sanz-Novo, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Laura Colzi, Shaoshan Zeng, Andrés Megías, Álvaro López-Gallifa, Antonio Martínez-Henares, Sarah Massalkhi, Belén Tercero, Pablo de Vicente, Sergio Martín, David San Andrés, Miguel A. Requena-Torres, José Luis Alonso
Figure caption: Transitions of conformer II of glycine (NH2CH2COOH) used to derive its column density upper limit. The observed spectrum is shown as a gray histogram, and the LTE synthetic model using the derived upper limit is shown with a red curve.
Paper: First Glycine Isomer Detected in the Interstellar Medium: Glycolamide (NH2C(O)CH2OH)
Authors: Víctor M. Rivilla, Miguel Sanz-Novo, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Laura Colzi, Shaoshan Zeng, Andrés Megías, Álvaro López-Gallifa, Antonio Martínez-Henares, Sarah Massalkhi, Belén Tercero, Pablo de Vicente, Sergio Martín, David San Andrés, Miguel A. Requena-Torres, José Luis Alonso
Figure caption: Transition of anti-glycolamide (anti-NH2C(O)CH2OH) used to derive its column density upper limit. The observed spectrum is shown as a gray histogram, and the LTE synthetic model using the derived upper limit is shown with a red curve.
Paper: First Glycine Isomer Detected in the Interstellar Medium: Glycolamide (NH2C(O)CH2OH)
Authors: Víctor M. Rivilla, Miguel Sanz-Novo, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Laura Colzi, Shaoshan Zeng, Andrés Megías, Álvaro López-Gallifa, Antonio Martínez-Henares, Sarah Massalkhi, Belén Tercero, Pablo de Vicente, Sergio Martín, David San Andrés, Miguel A. Requena-Torres, José Luis Alonso
Figure caption: Transitions of conformer I of glycine (NH2CH2COOH) used to derive its column density upper limit. The observed spectrum is shown as a gray histogram, and the LTE synthetic model using the derived upper limit is shown with a red curve.
Paper: First Glycine Isomer Detected in the Interstellar Medium: Glycolamide (NH2C(O)CH2OH)
Authors: Víctor M. Rivilla, Miguel Sanz-Novo, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Laura Colzi, Shaoshan Zeng, Andrés Megías, Álvaro López-Gallifa, Antonio Martínez-Henares, Sarah Massalkhi, Belén Tercero, Pablo de Vicente, Sergio Martín, David San Andrés, Miguel A. Requena-Torres, José Luis Alonso
Figure caption: Transition of syn-methyl carbamate (CH3OC(O)NH2) used to derive its column density upper limit. The observed spectrum is shown as a gray histogram, and the LTE synthetic model using the derived upper limit is shown with a red curve.
Paper: First Glycine Isomer Detected in the Interstellar Medium: Glycolamide (NH2C(O)CH2OH)
Authors: Víctor M. Rivilla, Miguel Sanz-Novo, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Laura Colzi, Shaoshan Zeng, Andrés Megías, Álvaro López-Gallifa, Antonio Martínez-Henares, Sarah Massalkhi, Belén Tercero, Pablo de Vicente, Sergio Martín, David San Andrés, Miguel A. Requena-Torres, José Luis Alonso
Figure caption: Transition of N-(Z)-hydroxyacetamide (CH3C(O)NHOH) used to derive its column density upper limit. The observed spectrum is shown as a gray histogram, and the LTE synthetic model using the derived upper limit is shown with a red curve.
Paper: A Broken “α–intensity” Relation Caused by the Evolving Photosphere Emission and the Nature of the Extraordinarily Bright GRB 230307A
Authors: Yun Wang, Zi-Qing Xia, Tian-Ci Zheng, Jia Ren, Yi-Zhong Fan
Figure caption: The E p,z–E  γ,iso diagram. The blue and gray points are the data of type I and type II GRBs with known redshifts, and the corresponding dashed lines represent the 2σ cor correlation regions, respectively (Minaev & Pozanenko 2020a, 2020b). Green markers represent the different phases of GRB 060614, the first long-duration burst (lasting about 100 s) with identified kilonova emission (Jin et al. 2015; Yang et al. 2015). Black markers represent another case of merger origin, GRB 211211A (Yang et al. 2022). The red circle and open inverted triangle are for GRB 230307A in the case of z = 0.065 and 3.87, respectively.
Paper: A Broken “α–intensity” Relation Caused by the Evolving Photosphere Emission and the Nature of the Extraordinarily Bright GRB 230307A
Authors: Yun Wang, Zi-Qing Xia, Tian-Ci Zheng, Jia Ren, Yi-Zhong Fan
Figure caption: Spectral lags of three episodes. The time bin size of episode a and episode b is set to 0.01 s. And because the duration of episode b is longer, its time bin size is set to 0.05 s. The error comes from the Monte Carlo simulation of the light curve.
Paper: A Broken “α–intensity” Relation Caused by the Evolving Photosphere Emission and the Nature of the Extraordinarily Bright GRB 230307A
Authors: Yun Wang, Zi-Qing Xia, Tian-Ci Zheng, Jia Ren, Yi-Zhong Fan
Figure caption: Framework of HEtools.
Paper: Two Candidate Obscured Tidal Disruption Events Coincident with High-energy Neutrinos
Authors: Ning Jiang, Ziying Zhou, Jiazheng Zhu, Yibo Wang, Tinggui Wang
Figure caption: The MIR and optical light curves of SDSSJ1048+1228 and SDSSJ1649+2625. The NEOWISE photometry in W1 (3.4 μm) and W2 (4.6 μm) band are shown as orange and brown squares while the blue and red triangles represent the 3σ  upper limits of ZTF forced difference photometry in the g and r bands. The vertical dashed lines mark the arrival time of matched high-energy neutrinos IceCube-200109A and IceCube-200530A.
Paper: Two Candidate Obscured Tidal Disruption Events Coincident with High-energy Neutrinos
Authors: Ning Jiang, Ziying Zhou, Jiazheng Zhu, Yibo Wang, Tinggui Wang
Figure caption: Sky map of observed high-energy neutrino event (Gold alerts) positions and their corresponding error region sizes, which are indicated by a color bar on the right. The footprint of SDSS, from which our MIRONG sample is selected, is overplotted in gray overlay. The objects in our MIRONG sample with IR peaks at the same period are denoted as red diamonds and those with W2 ≤ 12.60 are marked as dark red. The two sources that coincide with neutrinos are highlighted as red five-point stars. The clustering effect of the events around the equator region is due to the detector’s high sensitivity in this area.
Paper: Two Candidate Obscured Tidal Disruption Events Coincident with High-energy Neutrinos
Authors: Ning Jiang, Ziying Zhou, Jiazheng Zhu, Yibo Wang, Tinggui Wang
Figure caption: The optical spectra of SDSSJ1048+1228 and SDSSJ1649+2625. The archival SDSS spectrum is shown in orange, while the new spectrum taken after the outburst is shown in blue. No obvious spectral evolution is found for both objects.
Paper: Two Candidate Obscured Tidal Disruption Events Coincident with High-energy Neutrinos
Authors: Ning Jiang, Ziying Zhou, Jiazheng Zhu, Yibo Wang, Tinggui Wang
Figure caption: Left: the W2 variability amplitude (ΔW2) vs. redshift distribution of the MIRONG sources used to match with neutrinos. Right: the W2 magnitude vs. redshift distribution. The two sources coincident with neutrinos are highlighted by red five-point stars.
Paper: Rotational Flows in Solar Coronal Flux Rope Cavities
Authors: Valeriia Liakh, Rony Keppens
Figure caption: Temporal evolution of the total mass, angular momentum, and kinetic energy of the coronal and prominence plasma in the dynamically evolving and tracked FR region.
Paper: Outflowing Helium from a Mature Mini-Neptune
Authors: Michael Zhang, Fei Dai, Jacob L. Bean, Heather A. Knutson, Federica Rescigno
Figure caption: Relationship between the “observed” and “energy-limited” mass-loss rates, with mini-Neptunes highlighted in red (TOI 2134b) or blue (all others). Stripping off the constants, this is a relationship between R * W avg and F XUV/ρ XUV. For consistency with previous literature, we define XUV to be 5–504 Å. The dashed lines indicate what the relationship should be for 100% and 10% efficiency. Omitted for clarity is the very large (potentially OOM) uncertainty on the XUV flux, and therefore on the x-axis values, for all data points.
Paper: Outflowing Helium from a Mature Mini-Neptune
Authors: Michael Zhang, Fei Dai, Jacob L. Bean, Heather A. Knutson, Federica Rescigno
Figure caption: Left: average in-transit excess absorption in the planet rest frame. The deep silicon line at 10830 Å poses difficulties for spectral extraction and may be inherently variable, causing anomalies in the 0.6 Å surrounding that wavelength (gray region). Right: light curve of the helium line, defined as the region within 0.75 Å of 10833.3 Å in the stellar rest frame. This bandpass only captures the stronger peak. The two vertical lines mark the beginning and end of white-light transit.(The data used to create this figure are available.)
Paper: Outflowing Helium from a Mature Mini-Neptune
Authors: Michael Zhang, Fei Dai, Jacob L. Bean, Heather A. Knutson, Federica Rescigno
Figure caption: Reconstructed stellar spectrum.(The data used to create this figure are available.)
Paper: Outflowing Helium from a Mature Mini-Neptune
Authors: Michael Zhang, Fei Dai, Jacob L. Bean, Heather A. Knutson, Federica Rescigno
Figure caption: Version of Figure 3 where we attempt to estimate the metastable helium fraction instead of fixing it at 10−6. KELT-9b is far off the top of the chart.
Paper: Outflowing Helium from a Mature Mini-Neptune
Authors: Michael Zhang, Fei Dai, Jacob L. Bean, Heather A. Knutson, Federica Rescigno
Figure caption: Percent excess absorption (relative to median) as a function of time and wavelength while the planet was days away from transit. This figure is of the same format and has the same wavelength range and color bar scale as Figure 1.
Paper: Outflowing Helium from a Mature Mini-Neptune
Authors: Michael Zhang, Fei Dai, Jacob L. Bean, Heather A. Knutson, Federica Rescigno
Figure caption: Light curve of the helium line (within a half-width of 0.75 Å) while the planet was far from transit. This figure is the analog of Figure 2 (right), and the y-axis has the same scale.
Paper: Outflowing Helium from a Mature Mini-Neptune
Authors: Michael Zhang, Fei Dai, Jacob L. Bean, Heather A. Knutson, Federica Rescigno
Figure caption: Stellar spectrum in the terrestrial frame before and after correction for telluric absorption.
Paper: Outflowing Helium from a Mature Mini-Neptune
Authors: Michael Zhang, Fei Dai, Jacob L. Bean, Heather A. Knutson, Federica Rescigno
Figure caption: Best fit from our Parker wind model compared to the data and residuals.
Paper: Outflowing Helium from a Mature Mini-Neptune
Authors: Michael Zhang, Fei Dai, Jacob L. Bean, Heather A. Knutson, Federica Rescigno
Figure caption: The 2D posteriors from nested sampling for the Parker wind model.
Paper: Orbital Decay in an Accreting and Eclipsing 13.7 Minute Orbital Period Binary with a Luminous Donor
Authors: Kevin B. Burdge, Kareem El-Badry, Saul Rappaport, Tin Long Sunny Wong, Evan B. Bauer, Lars Bildsten, Ilaria Caiazzo, Deepto Chakrabarty, Emma Chickles, Matthew J. Graham, Erin Kara, S. R. Kulkarni, Thomas R. Marsh, Melania Nynka, Thomas A. Prince, Robert A. Simcoe, Jan van Roestel, Zach Vanderbosch, Eric C. Bellm, Richard G. Dekany, Andrew J. Drake, George Helou, Frank J. Masci, Jennifer Milburn, Reed Riddle, Ben Rusholme, Roger Smith
Figure caption: Model fit of the binned CHIMERA ﹩g^{\prime} ﹩ light curve of ZTF J0127+5258. We used the LCURVE modeling code to construct a physical model for the system. In order to account for the behavior in the light curve, particularly the geometry of the eclipses, as well as the increased flux at the quadrature phase at 0.75, we had to include an accretion disk with a bright spot, indicating that the disk and bright spot contribute an appreciable fraction of the optical flux.
Paper: Orbital Decay in an Accreting and Eclipsing 13.7 Minute Orbital Period Binary with a Luminous Donor
Authors: Kevin B. Burdge, Kareem El-Badry, Saul Rappaport, Tin Long Sunny Wong, Evan B. Bauer, Lars Bildsten, Ilaria Caiazzo, Deepto Chakrabarty, Emma Chickles, Matthew J. Graham, Erin Kara, S. R. Kulkarni, Thomas R. Marsh, Melania Nynka, Thomas A. Prince, Robert A. Simcoe, Jan van Roestel, Zach Vanderbosch, Eric C. Bellm, Richard G. Dekany, Andrew J. Drake, George Helou, Frank J. Masci, Jennifer Milburn, Reed Riddle, Ben Rusholme, Roger Smith
Figure caption: Extinction-corrected optical spectrum of ZTF J0127+5258 obtained with LRIS on the Keck I telescope. Much like the spectrum of PTF J0533+0209 (Burdge et al. 2019b), the atmosphere of the donor exhibits a mixture of hydrogen and helium absorption lines, indicating that it is helium-rich but still contains traces of hydrogen. Because of the contribution of the accretion disk to both the continuum and the dilution of the absorption lines by emission, we do not fit a model atmosphere to the object. Instead, we use the spectral energy distribution (SED) to estimate the temperature of the object.
Paper: Orbital Decay in an Accreting and Eclipsing 13.7 Minute Orbital Period Binary with a Luminous Donor
Authors: Kevin B. Burdge, Kareem El-Badry, Saul Rappaport, Tin Long Sunny Wong, Evan B. Bauer, Lars Bildsten, Ilaria Caiazzo, Deepto Chakrabarty, Emma Chickles, Matthew J. Graham, Erin Kara, S. R. Kulkarni, Thomas R. Marsh, Melania Nynka, Thomas A. Prince, Robert A. Simcoe, Jan van Roestel, Zach Vanderbosch, Eric C. Bellm, Richard G. Dekany, Andrew J. Drake, George Helou, Frank J. Masci, Jennifer Milburn, Reed Riddle, Ben Rusholme, Roger Smith
Figure caption: Our fit of the SED of ZTF J0127+5258 using a composite blackbody model. We constrained the accretor and donor luminosity to have a ratio of 1 ± 0.1 at 4770 Å  based on the depth of the primary eclipse seen in the CHIMERA ﹩g^{\prime} ﹩ light curve.
Paper: Orbital Decay in an Accreting and Eclipsing 13.7 Minute Orbital Period Binary with a Luminous Donor
Authors: Kevin B. Burdge, Kareem El-Badry, Saul Rappaport, Tin Long Sunny Wong, Evan B. Bauer, Lars Bildsten, Ilaria Caiazzo, Deepto Chakrabarty, Emma Chickles, Matthew J. Graham, Erin Kara, S. R. Kulkarni, Thomas R. Marsh, Melania Nynka, Thomas A. Prince, Robert A. Simcoe, Jan van Roestel, Zach Vanderbosch, Eric C. Bellm, Richard G. Dekany, Andrew J. Drake, George Helou, Frank J. Masci, Jennifer Milburn, Reed Riddle, Ben Rusholme, Roger Smith
Figure caption: Measured evolution of eclipse times in ZTF J0127+5258. The red fit of a quadratic clearly indicates that the system is undergoing orbital decay, as the coefficient of the quadratic term of the polynomial is clearly negative. A precise measurement of the orbital evolution was made possible by the eclipsing nature of the source (allowing for precise timing) and the long baseline resulting from archival PTF and ATLAS observations.
Paper: Orbital Decay in an Accreting and Eclipsing 13.7 Minute Orbital Period Binary with a Luminous Donor
Authors: Kevin B. Burdge, Kareem El-Badry, Saul Rappaport, Tin Long Sunny Wong, Evan B. Bauer, Lars Bildsten, Ilaria Caiazzo, Deepto Chakrabarty, Emma Chickles, Matthew J. Graham, Erin Kara, S. R. Kulkarni, Thomas R. Marsh, Melania Nynka, Thomas A. Prince, Robert A. Simcoe, Jan van Roestel, Zach Vanderbosch, Eric C. Bellm, Richard G. Dekany, Andrew J. Drake, George Helou, Frank J. Masci, Jennifer Milburn, Reed Riddle, Ben Rusholme, Roger Smith
Figure caption: Measured radial velocities of the hydrogen absorption lines in the spectrum of ZTF J0127+5258. The orbital phases are referenced to those determined from the mid-eclipse time in the light-curve model. The poor fit near inferior conjunction (phase 0.5) may originate from a Rossiter–McLaughlin effect as the accretion disk and accreting WD transit the donor.
Paper: Orbital Decay in an Accreting and Eclipsing 13.7 Minute Orbital Period Binary with a Luminous Donor
Authors: Kevin B. Burdge, Kareem El-Badry, Saul Rappaport, Tin Long Sunny Wong, Evan B. Bauer, Lars Bildsten, Ilaria Caiazzo, Deepto Chakrabarty, Emma Chickles, Matthew J. Graham, Erin Kara, S. R. Kulkarni, Thomas R. Marsh, Melania Nynka, Thomas A. Prince, Robert A. Simcoe, Jan van Roestel, Zach Vanderbosch, Eric C. Bellm, Richard G. Dekany, Andrew J. Drake, George Helou, Frank J. Masci, Jennifer Milburn, Reed Riddle, Ben Rusholme, Roger Smith
Figure caption: Phase-folded ATLAS and PTF light curves of ZTF J0127+5258 (note that this phase fold accounts for both the period and period derivative). In red, we overplot the light-curve model used to time the system and measure the orbital period derivative.
Paper: Rotational Flows in Solar Coronal Flux Rope Cavities
Authors: Valeriia Liakh, Rony Keppens
Figure caption: Time–distance diagram of the density along selected field lines (top) and poloidal field projected v ∥ at the center of mass of the same field lines (bottom). Left: the temporal evolution for the field lines with the dip at the height y = 12.8  Mm and radius of curvature R  c  = 3.0  Mm. Right: for the field line with the dip at height y = 10.8  Mm and radius of curvature R  c  = 5.2  Mm. The green lines in panels (a) and (c) denote the position of the corresponding magnetic dip.
Paper: Orbital Decay in an Accreting and Eclipsing 13.7 Minute Orbital Period Binary with a Luminous Donor
Authors: Kevin B. Burdge, Kareem El-Badry, Saul Rappaport, Tin Long Sunny Wong, Evan B. Bauer, Lars Bildsten, Ilaria Caiazzo, Deepto Chakrabarty, Emma Chickles, Matthew J. Graham, Erin Kara, S. R. Kulkarni, Thomas R. Marsh, Melania Nynka, Thomas A. Prince, Robert A. Simcoe, Jan van Roestel, Zach Vanderbosch, Eric C. Bellm, Richard G. Dekany, Andrew J. Drake, George Helou, Frank J. Masci, Jennifer Milburn, Reed Riddle, Ben Rusholme, Roger Smith
Figure caption: Mass transfer rate (top), donor effective temperature (middle), and period derivative (bottom) as a function of the orbital period. Colored lines show He WD models labeled by the initial central specific entropy of the donor in units of N A k B, whereas the gray line shows a He star model similar to the 0.37 M ⊙ model in Bauer & Kupfer (2021). The observed properties of ZTF J0127+5258 are shown with blue lines with uncertainties bracketed by blue shaded regions. For the He WD 4.0 model, we show the full evolution past period minimum, with arrows in the top panel indicating the flow of time. For this model, we also show the estimated effects of tidal heating by adding ﹩{\dot{E}}_{\mathrm{tide}}﹩ (dashed line) or ﹩{\dot{E}}_{\mathrm{heat}}﹩ (dotted–dashed line) to the intrinsic luminosity of the model and recalculating the effective temperature via the Stefan–Boltzmann law.
Paper: Orbital Decay in an Accreting and Eclipsing 13.7 Minute Orbital Period Binary with a Luminous Donor
Authors: Kevin B. Burdge, Kareem El-Badry, Saul Rappaport, Tin Long Sunny Wong, Evan B. Bauer, Lars Bildsten, Ilaria Caiazzo, Deepto Chakrabarty, Emma Chickles, Matthew J. Graham, Erin Kara, S. R. Kulkarni, Thomas R. Marsh, Melania Nynka, Thomas A. Prince, Robert A. Simcoe, Jan van Roestel, Zach Vanderbosch, Eric C. Bellm, Richard G. Dekany, Andrew J. Drake, George Helou, Frank J. Masci, Jennifer Milburn, Reed Riddle, Ben Rusholme, Roger Smith
Figure caption: Diagram of the possible outcomes of double white dwarf mergers presented in Shen (2015), with the dashed blue lines indicating the mass constraints on ZTF J0127+5258 in the low mass transfer rate case and the dashed green lines indicating the constraints in the high mass transfer rate case. If ZTF J0127+5258 fails to undergo stable mass transfer and evolve into a helium CV, this diagram indicates that it will likely form an R CrB star that eventually cools into a white dwarf if its current mass transfer rate is on the lower end of our estimates or explode as a Type Ia supernova if its mass transfer rate is on the higher end of our estimates. Note that parenthetical entries in the merger outcomes may not apply to all objects in that mass range.