adsabs/AstroCLIMB huggingface dataset:
Paper: A γ-Ray-emitting Collisional Ring Galaxy System in Our Galactic Neighborhood
Authors: Vaidehi S. Paliya, D. J. Saikia
Figure caption: Top left: DECAM g-band image of “Kathryn’s Wheel.” The brightest pixels were masked, and the color scale was adjusted to enhance the faint features. Top right: Swift-XRT counts map of the same region. The red circles represent the identified X-ray sources and have a radius of 5.″6, estimated as the positional uncertainty in the optimized X-ray positions. The green contours refer to the 1.36 GHz emission observed by RACS. The contours start at three×rms and increase in the multiple of ﹩\sqrt{1.5}﹩. Bottom: the same as the top panels but zooming in on the system. Here, we have used DECAM VR-band data with a longer exposure than the g-band image. The radio contours are shown in white for clarity. North is up and east to the left.
Paper: A γ-Ray-emitting Collisional Ring Galaxy System in Our Galactic Neighborhood
Authors: Vaidehi S. Paliya, D. J. Saikia
Figure caption: This plot shows the γ-ray luminosity as a function of infrared luminosity for γ-ray-detected (red circles) and undetected (blue squares) star-forming galaxies. For Fermi-LAT undetected sources, the γ-ray luminosities are upper limits. The black solid line and green shaded region refer to the best-fitted correlation and 1σ uncertainty, respectively, reported by Ajello et al. (2020). The location of “Kathryn’s Wheel” system is shown with a black star. The black pentagon shows the case when all of the γ-ray emission is considered to be originating from the dwarf galaxy LEDA 3080069 alone.
Paper: A γ-Ray-emitting Collisional Ring Galaxy System in Our Galactic Neighborhood
Authors: Vaidehi S. Paliya, D. J. Saikia
Figure caption: Left: the continuum-subtracted Hα image of the collisional ring galaxy system. We overplot the 1.36 GHz RACS contours to highlight the cospatiality of the star-forming regions and the radio emission. Right: the W2-band image of the system taken with Swift-UVOT. The overplotted Hα contours (representing the star-forming regions shown in the left panel) reveal that the cospatial bright UV emission likely originated from the massive hot stars. North is up and east to the left.
Paper: A γ-Ray-emitting Collisional Ring Galaxy System in Our Galactic Neighborhood
Authors: Vaidehi S. Paliya, D. J. Saikia
Figure caption: The 0.′8 × 0.′8 VIMOS-VLT image of the dwarf galaxy LEDA 3080069 centered at R.A. = 251.°8667055, and decl. = −57.°4258147 (J2000). North is up and east to the left.
Paper: Resonance of Low-frequency Electromagnetic and Ion-sound Modes in the Solar Wind
Authors: I. Y. Vasko, F. S. Mozer, T. Bowen, J. Verniero, X. An, A. V. Artemyev, S. D. Bale, J. W. Bonnell, J. Halekas, I. V. Kuzichev
Figure caption: The properties of low-frequency, bandpass filtered over 2–6 Hz, electric and magnetic fields. For each 10 s subinterval of about 20 minute interval we computed (a) the best-fit slopes for E  X  vs. B  Y  and E  Y  vs B  X , Alfvén speed v  A , and ﹩\hat{{\boldsymbol{k}}}\cdot {{\boldsymbol{V}}}_{i};﹩ the latter is the ion flow velocity component along unit vector ﹩\hat{{\boldsymbol{k}}}﹩ that is the propagation direction of the low-frequency electromagnetic fluctuations; (b) the wave normal angle between ﹩\hat{{\boldsymbol{k}}}﹩ and local background magnetic field; (c) plasma and spacecraft frame frequencies corresponding to the maximum power spectral density and (d) the corresponding wavenumber. The frequencies and wavenumbers are normalized to local ion-cyclotron frequency f  ci  and ion inertial length λ  i , respectively.
Paper: Resonance of Low-frequency Electromagnetic and Ion-sound Modes in the Solar Wind
Authors: I. Y. Vasko, F. S. Mozer, T. Bowen, J. Verniero, X. An, A. V. Artemyev, S. D. Bale, J. W. Bonnell, J. Halekas, I. V. Kuzichev
Figure caption: Overview of PSP observations on 2019 April 1: (a) the magnetic field measured at about 146 S s−1 resolution and (b) the ion flow velocity provided at 0.2 s cadence; (c) the mean of power spectral densities (PSD) of magnetic field components in the XY plane and (d) the PSD of the magnetic field component along the Z-axis that is directed radially toward the Sun; (e) the mean of PSDs of electric field components in the XY plane; (f), (g) omnidirectional spectra of three magnetic and two electric field components averaged over about 20 minute and 3 s intervals. Note that the instrumental noise at about 8, 16, and 32 Hz noticeable in panel (d) has been removed in panels (f) and (g). The PSDs were computed using the fast Fourier transform with a 5 s sliding window and Hanning window function.
Paper: Resonance of Low-frequency Electromagnetic and Ion-sound Modes in the Solar Wind
Authors: I. Y. Vasko, F. S. Mozer, T. Bowen, J. Verniero, X. An, A. V. Artemyev, S. D. Bale, J. W. Bonnell, J. Halekas, I. V. Kuzichev
Figure caption: An expanded view of electric and magnetic fields measured over a 3 s interval: (a) waveforms of two electric field components measured at about 293 S s−1 resolution; (b) low-frequency and (c) high-frequency electric field fluctuations computed by bandpass filtering the electric field over 2–6 Hz and 6–146 Hz; (d) similarly computed low-frequency magnetic field. Panels (e) and (f) compare low-frequency electric and magnetic fields in the XY plane, and indicate the best-fit slopes for E  X  vs. B  Y  and E  Y  vs. B  X .
Paper: Phosphorus Enrichment by ONe Novae in the Galaxy
Authors: Kenji Bekki, Takuji Tsujimoto
Figure caption: Distribution of the Galactic P-normal stars with [P/Fe] < 1 on the [Fe/H]−[P/Fe] plane and illustration of the predicted evolutionary path of the “ONe nova” scenario (wide gray line). Observational results for P-normal stars ([P/Fe] < 1) from (i) Roederer et al. (2014, 2016), (ii) Maas et al. (2022), and (iii) Caffau et al. (2016, 2019), M20, Maas et al. (2022), and Nandakumar et al. (2022) are plotted by filled circles, open circles, and crosses, respectively. The gray line just illustrates how [P/Fe] evolves with [Fe/H]: the exact details of the evolutionary paths (e.g., [Fe/H] at the maximum [P/Fe]) from the present chemical evolution model can be different from this line. Characteristic features of the models are explained with short phrases at appropriate places (e.g., “CCSN only” at [Fe/H]< −2.4).
Paper: Phosphorus Enrichment by ONe Novae in the Galaxy
Authors: Kenji Bekki, Takuji Tsujimoto
Figure caption: Evolutionary paths of four models with M ej = 1 × 10−4 M ⊙ (blue solid), 2 × 10−4 M ⊙ (purple dotted), 4 × 10−4 M ⊙ (dark blue dashed; fiducial model), and 6 × 10−4 M ⊙ (orange dotted–dashed) on the [Fe/H]–[P/Fe] plane. These models adopt (i) [Fe/H]-dependent N ONe (α Z = 3 × 10−3), (ii) N ONe,0 = 0.01, and (iii) fixed mass fraction of P in ejecta of CCSNe for the adopted Salpeter IMF (﹩{f}_{{\rm{P}},\mathrm{CCSN}}=1.1\times {10}^{-5}﹩ and β Z = 0). Small black dots are observational data taken from Figure 1.
Paper: Phosphorus Enrichment by ONe Novae in the Galaxy
Authors: Kenji Bekki, Takuji Tsujimoto
Figure caption: Same as Figure 2 but for four models with α Z = −1.7 × 10−3 and N ONe,0 = 0.01 (blue solid), α Z = −2.7 × 10−3 and N ONe,0 = 0.01, (purple dotted), α Z = 0 and N ONe,0 = 0.01, (dark blue dashed), and α Z = −1.3 × 10−3 and N ONe,0 = 0.003, (orange dotted–dashed). Only the last model has a different N ONe, 0 from other three in this figure and those in Figure 2. Other model parameters in the four are exactly the same as those in the fiducial model.
Paper: Phosphorus Enrichment by ONe Novae in the Galaxy
Authors: Kenji Bekki, Takuji Tsujimoto
Figure caption: Evolutionary paths of four models with ﹩{f}_{\mathrm{Cl},\mathrm{CCSN}}=2.4\times {10}^{-6}﹩ (blue solid), 4.7 × 10−6 (purple dotted), 9.4 × 10−6 (dark blue dashed), and 1.4 × 10−5 (orange dotted–dashed) on the [Fe/H]−[Cl/Fe] plane. In these models, all other parameter values are exactly the same as those in the fiducial model. Observational data points for stars with T eff > 3500 K from Maas & Pilachowski (2021) are plotted by small black dots.
Paper: Phosphorus Enrichment by ONe Novae in the Galaxy
Authors: Kenji Bekki, Takuji Tsujimoto
Figure caption: Same as Figure 2 but for four models with different slopes of metallicity-dependent P yields of CCSNe, i.e., β Z = 4 × 10−3 (blue solid), β Z = 2 × 10−3, (purple dotted), β Z = 1 × 10−3, (dark blue dashed), and β Z = 0 (orange dotted–dashed; no metallicity dependence of P yields).
Paper: Dracula’s Chivito: Discovery of a Large Edge-on Protoplanetary Disk with Pan-STARRS
Authors: Ciprian T. Berghea, Ammar Bayyari, Michael L. Sitko, Jeremy J. Drake, Ana Mosquera, Cecilia Garraffo, Thomas Petit, Ray W. Russell, Korash D. Assani
Figure caption: (a) Color (giy bands) PS1 image of DraChi. The coordinates of the center of the disk are R. A. = 347.°432214, decl. = 67.°394451. In the northern part of the disk, very faint filaments are seen extending 17″ out from both edges of the disk. In the south these features, which we call “fangs” in the text, are likely not visible because of increased extinction. (b) The best radiative transfer model image in the same bands. The model image was convolved with the PS1 PSF. The “edges” of the envelope are very similar to the faint fangs in panel a. (c) PS1 r-band image with contours to show the faint fangs. The blue circle has a radius of 16″. (d) PS1 r-band image showing the analysis of the scattered light. The blue lines are spines fitted to the two lobes as described in the text, and the peaks of the emission are marked with a dot. A significant lateral asymmetry can be clearly seen, suggesting a tilted inner region.
Paper: Jupiter Co-Orbital Comet P/2023 V6 (PANSTARRS): Orbital History and Modern Activity State
Authors: Theodore Kareta, John W. Noonan, Kathryn Volk, Ryder H. Strauss, David Trilling
Figure caption: The orbital evolution of V6 between the years 2010 and 2050 is shown, along with that of 1000 orbital “clones” consistent with the object’s orbit as described in the text. Top: the evolution of the difference in orbital longitude of V6 and Jupiter is shown in black. Stable values of this angular difference (e.g., where the curves are approximately “flat”) are when the two objects have very similar orbital periods and are thus co-orbital. Middle: the evolution of V6's semimajor axis (a) in blue and perihelion (q) in orange are shown. Bottom: the distance between the comet and Jupiter is plotted in black. The sudden jumps in q and a, like those in 2020, 2032, and 2044, are from close encounters with Jupiter. The 2044 encounter is by far the deepest where the common path of the clones diverges due to cumulative uncertainties in the object’s orbit becoming substantial and is discussed at length in the text.
Paper: Jupiter Co-Orbital Comet P/2023 V6 (PANSTARRS): Orbital History and Modern Activity State
Authors: Theodore Kareta, John W. Noonan, Kathryn Volk, Ryder H. Strauss, David Trilling
Figure caption: Left: a stack of a subset of our LDT/LMI imaging of V6 on 2023 November 22 totaling 3120 s (or ∼0.86 hr) shown in a logarithmic stretch between the peak brightness of the comet and 2% of it. A legend in the lower left shows the direction toward the Sun (indicated with a yellow circle-dot symbol) and the direction opposite the object's velocity (denoted with a −v). Right: spatial cuts along the comet’s velocity axis of the left panel image are shown, highlighting the comet’s weak but clear extension in its antivelocity direction. The low phase angle and moderate heliocentric distance of these observations mean that most of the tail is radially away from the observer. As mentioned in the text, the leading profile of the spatial cut can be fit with a power law of slope −0.9 ± 0.2, consistent with the expectation for a comet with relatively stable activity.
Paper: Jupiter Co-Orbital Comet P/2023 V6 (PANSTARRS): Orbital History and Modern Activity State
Authors: Theodore Kareta, John W. Noonan, Kathryn Volk, Ryder H. Strauss, David Trilling
Figure caption: The evolution of heliocentric distances R  H  for V6 (black) and LD2 (orange) are shown. Two dashed vertical lines are added in the same colors to indicate at what heliocentric distances their Af ρ values were measured, with same-colored stars placed above the intersection with the R  H  curves. The two objects were both observed shortly after their first perihelion passage after becoming co-orbital, and they both were previously in colder orbits exterior to Jupiter. The similarities begin to end one orbital period after their close encounters, as LD2 is scattered outward (the sudden change in direction it undergoes in 2028) while V6 is moved into a lower-eccentricity orbit that is then scattered outward one orbital period after that.
Paper: Jupiter Co-Orbital Comet P/2023 V6 (PANSTARRS): Orbital History and Modern Activity State
Authors: Theodore Kareta, John W. Noonan, Kathryn Volk, Ryder H. Strauss, David Trilling
Figure caption: A long-term integration of V6 and 100 orbital clones is shown, essentially a “zoom-out” of the bottom panel of Figure 2, with V6's perihelion, semimajor axis, and aphelion plotted in orange, black, and blue respectively. The object’s 2022–2044 co-orbital status is bookended by long periods where the object has a perihelion in the vicinity of Jupiter’s orbit but with a significantly larger semimajor axis than its current value. The orbital integrations begin to decohere prior to a close encounter with Jupiter in ∼1942 and after a close encounter with Jupiter in ∼2067.
Paper: Dracula’s Chivito: Discovery of a Large Edge-on Protoplanetary Disk with Pan-STARRS
Authors: Ciprian T. Berghea, Ammar Bayyari, Michael L. Sitko, Jeremy J. Drake, Ana Mosquera, Cecilia Garraffo, Thomas Petit, Ray W. Russell, Korash D. Assani
Figure caption: Average extinctions for Gaia stars within 3° of DraChi.
Paper: Dracula’s Chivito: Discovery of a Large Edge-on Protoplanetary Disk with Pan-STARRS
Authors: Ciprian T. Berghea, Ammar Bayyari, Michael L. Sitko, Jeremy J. Drake, Ana Mosquera, Cecilia Garraffo, Thomas Petit, Ray W. Russell, Korash D. Assani
Figure caption: SED constructed with all the data presented in this Letetr and our best HOCHUNK3D model. We also show the extincted model with A  V  = 0.95 (dashed line). The optical spectrum was scaled to match the PS1 r band. Most error bars (formal errors) are too small to be visible.
Paper: Dracula’s Chivito: Discovery of a Large Edge-on Protoplanetary Disk with Pan-STARRS
Authors: Ciprian T. Berghea, Ammar Bayyari, Michael L. Sitko, Jeremy J. Drake, Ana Mosquera, Cecilia Garraffo, Thomas Petit, Ray W. Russell, Korash D. Assani
Figure caption: Template best fit to the optical spectrum of DraChi. The spectrum was dereddened by A  V  = 0.95.
Paper: JWST/NIRCam Detection of the Fomalhaut C Debris Disk in Scattered Light
Authors: Kellen Lawson, Joshua E. Schlieder, Jarron M. Leisenring, Ell Bogat, Charles A. Beichman, Geoffrey Bryden, András Gáspár, Tyler D. Groff, Michael W. McElwain, Michael R. Meyer, Thomas Barclay, Per Calissendorff, Matthew De Furio, Yiting Li, Marcia J. Rieke, Marie Ygouf, Thomas P. Greene, Julien H. Girard, Mario Gennaro, Jens Kammerer, Armin Rest, Thomas L. Roellig, Ben Sunnquist
Figure caption: Deprojected radial surface brightness profiles for MCRDI reductions of the F356W (left) and F444W (right) data. In each subplot, the profiles for the data, convolved model, and raw model are indicated by the solid blue line, solid orange line, and dotted orange line, respectively. The dashed gray line shows the 5σ noise level for the data. While the data and convolved model are in good agreement for F356W, for F444W the data show a deficit at and interior to the disk peak (likely a PSF subtraction effect) and are significantly more radially extended (discussed in Section 6).
Paper: JWST/NIRCam Detection of the Fomalhaut C Debris Disk in Scattered Light
Authors: Kellen Lawson, Joshua E. Schlieder, Jarron M. Leisenring, Ell Bogat, Charles A. Beichman, Geoffrey Bryden, András Gáspár, Tyler D. Groff, Michael W. McElwain, Michael R. Meyer, Thomas Barclay, Per Calissendorff, Matthew De Furio, Yiting Li, Marcia J. Rieke, Marie Ygouf, Thomas P. Greene, Julien H. Girard, Mario Gennaro, Jens Kammerer, Armin Rest, Thomas L. Roellig, Ben Sunnquist
Figure caption: Left: NIRCam F356W detection of the Fomalhaut C debris disk in scattered light resulting from the MCRDI procedure (Section 4). The image has been smoothed by a Gaussian kernel with FWHM of 6.7 pixels (3 × the PSF FWHM). The inner software mask has a radius of 1.″5 and covers the region of significant residual speckle noise. Logarithmically spaced black contours are drawn above the maximum for the color stretch to show the peak location of the bright southwestern background source. Right: same as the image on the left, but with silver contours showing the 1σ–5σ levels for the ALMA detection of the disk reported in Cronin-Coltsmann et al. (2021). The gold arrows extend from the locations of the two assumed background sources modeled in Cronin-Coltsmann et al. (2021), showing their expected displacement due to the proper motion of Fomalhaut C (Gaia Collaboration et al. 2023). Both predicted positions are consistent with sources detected in the 2022 NIRCam data, supporting their identity as unassociated background objects.
Paper: JWST/NIRCam Detection of the Fomalhaut C Debris Disk in Scattered Light
Authors: Kellen Lawson, Joshua E. Schlieder, Jarron M. Leisenring, Ell Bogat, Charles A. Beichman, Geoffrey Bryden, András Gáspár, Tyler D. Groff, Michael W. McElwain, Michael R. Meyer, Thomas Barclay, Per Calissendorff, Matthew De Furio, Yiting Li, Marcia J. Rieke, Marie Ygouf, Thomas P. Greene, Julien H. Girard, Mario Gennaro, Jens Kammerer, Armin Rest, Thomas L. Roellig, Ben Sunnquist
Figure caption: PSF-subtracted final images of Fomalhaut C in F356W (top row) and F444W (bottom row), as well as the MCRDI disk model and disk model residuals (two rightmost columns). To reduce noise, each image has been median binned by a factor of 5 (such that each pixel in the binned image is the median of a 5 × 5 pixel square in the original image). The first three columns correspond to the three PSF subtraction strategies (Section 4): classical RDI, SRDI, and MCRDI, respectively. The dashed ellipses mark the approximate shape and size of the disk identified by Cronin-Coltsmann et al. (2021).
Paper: JWST/NIRCam Detection of the Fomalhaut C Debris Disk in Scattered Light
Authors: Kellen Lawson, Joshua E. Schlieder, Jarron M. Leisenring, Ell Bogat, Charles A. Beichman, Geoffrey Bryden, András Gáspár, Tyler D. Groff, Michael W. McElwain, Michael R. Meyer, Thomas Barclay, Per Calissendorff, Matthew De Furio, Yiting Li, Marcia J. Rieke, Marie Ygouf, Thomas P. Greene, Julien H. Girard, Mario Gennaro, Jens Kammerer, Armin Rest, Thomas L. Roellig, Ben Sunnquist
Figure caption: Left: radial 5σ companion detection limits for MCRDI and SRDI reductions as a function of angular separation in arcsec (lower x-axis) and projected separation in au (upper x-axis). Limits are provided in terms of contrast with the host star (top left) and companion mass (bottom left). Right: companion detection probabilities for the F444W (4.4 μm) MCRDI reduction as a function of semimajor axis (for circular orbits coplanar with the disk) and companion mass (Jupiter masses on the left axis, and Earth masses on the right axis). White contours mark the 68%, 95%, and 99.7% probability thresholds. For context, the best-fit disk radius of 24.5 au is indicated by a vertical dashed line. These data effectively rule out companions more massive than ∼0.3M J in the vicinity of the disk.
Paper: JWST/NIRCam Detection of the Fomalhaut C Debris Disk in Scattered Light
Authors: Kellen Lawson, Joshua E. Schlieder, Jarron M. Leisenring, Ell Bogat, Charles A. Beichman, Geoffrey Bryden, András Gáspár, Tyler D. Groff, Michael W. McElwain, Michael R. Meyer, Thomas Barclay, Per Calissendorff, Matthew De Furio, Yiting Li, Marcia J. Rieke, Marie Ygouf, Thomas P. Greene, Julien H. Girard, Mario Gennaro, Jens Kammerer, Armin Rest, Thomas L. Roellig, Ben Sunnquist
Figure caption: Left: contrast curves for the nominal (dotted lines) and corrected (dashed lines) SRDI reductions of the Fomalhaut C data. The implemented corrections improve contrasts by up to a factor of six for both filters. Right: a comparison of synthetic PSF models for one roll of Fomalhaut C F356W data without (top row) and with (bottom row) the empirical corrections described in Appendix C. All images were divided by the radial average for the data to better compare the speckle patterns at all separations. The field of view for each panel is 2″ × 2″.
Paper: JWST/NIRCam Detection of the Fomalhaut C Debris Disk in Scattered Light
Authors: Kellen Lawson, Joshua E. Schlieder, Jarron M. Leisenring, Ell Bogat, Charles A. Beichman, Geoffrey Bryden, András Gáspár, Tyler D. Groff, Michael W. McElwain, Michael R. Meyer, Thomas Barclay, Per Calissendorff, Matthew De Furio, Yiting Li, Marcia J. Rieke, Marie Ygouf, Thomas P. Greene, Julien H. Girard, Mario Gennaro, Jens Kammerer, Armin Rest, Thomas L. Roellig, Ben Sunnquist
Figure caption: A comparison of the initial and corrected images from the background model subtraction procedure (Appendix A) for one science exposure (top row) and one reference exposure (bottom row) in F356W. The images of each row are normalized to the initial stellar PSF brightness to highlight the difference between the backgrounds (visible as initially more negative regions within the neutral density squares at the corners). The rightmost column shows the background model that is subtracted from the initial image.
Paper: Emergence of Microphysical Bulk Viscosity in Binary Neutron Star Postmerger Dynamics
Authors: Elias R. Most, Alexander Haber, Steven P. Harris, Ziyuan Zhang, Mark G. Alford, Jorge Noronha
Figure caption: Effective inverse Reynolds number ﹩\chi \equiv {\rm{\Pi }}/\left({e}^{\mathrm{eq}}+{P}^{\mathrm{eq}}\right)﹩ and density-averaged chemical potential difference δ μ normalized by the temperature T at times t relative to the time of merger t mer.
Paper: Emergence of Microphysical Bulk Viscosity in Binary Neutron Star Postmerger Dynamics
Authors: Elias R. Most, Alexander Haber, Steven P. Harris, Ziyuan Zhang, Mark G. Alford, Jorge Noronha
Figure caption: Chemical potential imbalance δ μ (normalized by the temperature T) as a measure of out-of-β-equilibrium effects during the merger and postmerger phases of two neutron stars when using the SFHo EoS with Urca processes (the orbital plane is shown). The green contours denote the rest-mass density of the merger remnant in units of nuclear saturation. All times, t, are stated relative to the time of merger t mer.
Paper: Emergence of Microphysical Bulk Viscosity in Binary Neutron Star Postmerger Dynamics
Authors: Elias R. Most, Alexander Haber, Steven P. Harris, Ziyuan Zhang, Mark G. Alford, Jorge Noronha
Figure caption: Distribution over density of electron fractions, Y  e , present in the system at time t = 5 ms after merger. Shown are the results for the simulations using the SFHo (top) and TMA (bottom) EoSs, with and without Urca processes.
Paper: Emergence of Microphysical Bulk Viscosity in Binary Neutron Star Postmerger Dynamics
Authors: Elias R. Most, Alexander Haber, Steven P. Harris, Ziyuan Zhang, Mark G. Alford, Jorge Noronha
Figure caption: Comparison of the Urca reaction timescale t Urca = 1/Γ to the sound-crossing time t sound, the gravitational-wave damping time t GW, and the timescale t  f2 of postmerger gravitational waves, about 6 ms after merger.
Paper: Emergence of Microphysical Bulk Viscosity in Binary Neutron Star Postmerger Dynamics
Authors: Elias R. Most, Alexander Haber, Steven P. Harris, Ziyuan Zhang, Mark G. Alford, Jorge Noronha
Figure caption: Gravitational-wave strain ﹩{h}_{+}^{22}﹩ (l = m = 2 component) for the merger performed using the TMA EoS. Different curves refer to various degrees of neutrino trapping. The bottom panel shows the frequency domain waveform around the dominant mode. A bulk viscous suppression in power for the Urca simulation is visible.