adsabs/AstroCLIMB huggingface dataset:
Paper: Abiotic Production of Dimethyl Sulfide, Carbonyl Sulfide, and Other Organosulfur Gases via Photochemistry: Implications for Biosignatures and Metabolic Potential
Authors: Nathan W. Reed, Randall L. Shearer, Shawn Erin McGlynn, Boswell A. Wing, Margaret A. Tolbert, Eleanor C. Browne
Figure caption: Chromatogram of organosulfur photochemical products from the 5 ppmv H2S and 0.1% CH4 in N2 gas mixture (red curve, left axis) as well as the DMS standard (blue curve, right axis).
Paper: Abiotic Production of Dimethyl Sulfide, Carbonyl Sulfide, and Other Organosulfur Gases via Photochemistry: Implications for Biosignatures and Metabolic Potential
Authors: Nathan W. Reed, Randall L. Shearer, Shawn Erin McGlynn, Boswell A. Wing, Margaret A. Tolbert, Eleanor C. Browne
Figure caption: Example output from the Multipeak Fit function in Igor Pro 8.04. The top chromatogram has both the sample chromatogram (red curve) and the fitted chromatogram done by the software (blue curve). The bottom plot shows the extracted and resolved peaks from the fit of the top chromatogram.
Paper: A Far-ultraviolet-detected Accretion Shock at the Star–Disk Boundary of FU Ori
Authors: Adolfo S. Carvalho, Lynne A. Hillenbrand, Kevin France, Gregory J. Herczeg
Figure caption: The corner plot for the fit with a variable T FUV, R eff, ﹩\dot{M}﹩, and A  V . The dark blue vertical and horizontal solid lines mark the median values of the histograms, while the light blue dotted lines mark the modal values. The agreement between the two in all but the T FUV parameter shows that the posterior distributions are well behaved. The contours in the 2D histogram mark the 0.5σ, 1.0σ, 1.5σ, and 2.0σ levels, while the vertical dashed lines mark the 16th and 84th percentiles in the 1D histograms.
Paper: A Far-ultraviolet-detected Accretion Shock at the Star–Disk Boundary of FU Ori
Authors: Adolfo S. Carvalho, Lynne A. Hillenbrand, Kevin France, Gregory J. Herczeg
Figure caption: The L FUV (this work) and L X (M. A. Kuhn & L. A. Hillenbrand 2019) for FU Ori, compared with YSOs in Taurus (H. Yang et al. 2012). FU Ori has among the highest L X and the highest L FUV of the sample. The range of L FUV for FU Ori reflects the two values we calculate depending on the assumed geometry of the emission region. The sources that have L FUV > 0.05 L ⊙ are T Tau, HD 143006, and RY Tau, which are much earlier spectral types than the FU Ori central object would be (K1, G3, and G0, respectively; G. J. Herczeg & L. A. Hillenbrand 2014).
Paper: A Far-ultraviolet-detected Accretion Shock at the Star–Disk Boundary of FU Ori
Authors: Adolfo S. Carvalho, Lynne A. Hillenbrand, Kevin France, Gregory J. Herczeg
Figure caption: Selected bright emission line doublets commonly studied in the FUV spectra of YSOs. The data are plotted in black, and the uncertainty on each point is shown in light gray. The blue and red lines mark the blue and red components of the doublets. The vertical cyan dashed lines mark the rest wavelengths of H2 lines, and the vertical magenta dotted lines mark the rest frequencies of known features that may be contaminating the doublet line profiles (Cl I 1351.657, Fe II 1352.487, and O IV] 1401.17).
Paper: A Far-ultraviolet-detected Accretion Shock at the Star–Disk Boundary of FU Ori
Authors: Adolfo S. Carvalho, Lynne A. Hillenbrand, Kevin France, Gregory J. Herczeg
Figure caption: The net counts in the COS G130M spectra from 1150 to 1200 Å. The λ cen = 1309 Å points are shown in maroon, and the λ cen = 1222 Å points are shown as dark blue squares. The counts have been resampled to a grid with 100 pixel wide bins. Prior to binning, we masked the spectrum following the procedure described in Section 2. We assume the uncertainties on each bin are Poisson-distributed. Notice that there are several bins with ∼10 counts, indicating a >3σ continuum emission detection.
Paper: A Far-ultraviolet-detected Accretion Shock at the Star–Disk Boundary of FU Ori
Authors: Adolfo S. Carvalho, Lynne A. Hillenbrand, Kevin France, Gregory J. Herczeg
Figure caption: Detected bright emission lines commonly seen in the FUV spectra of YSOs. The data are plotted in black, and the uncertainty on each point is shown in red. The rest frequency of each line is marked by the vertical gray line. Notice that, if present, the C I 1656 feature is only marginally detected.
Paper: Analyzing the Sequence of Phases Leading to the Formation of the Active Region 13664, with Potential Carrington-like Characteristics
Authors: P. Romano, A. Elmhamdi, A. Marassi, and L. Contarino
Figure caption: In the left panels a sequence of three HMI continuum images describing the main evolution of the AR 13664 before the X8.7 flare occurrence has been reported. The blue and red contours correspond to −500 and +500 G, respectively. Panel (d) displays the temporal evolution of the computed total unsigned magnetic flux (green) and the area in μHem covered by the sunspots forming the AR (dark-yellow dashed line). The central meridian passage (CMP) is highlighted by vertical short-dashed line. The curves start at 18:00 UT on 2024 May 2. The three arrows indicate the times when the images reported in panels (a), (b), and (c) have been acquired. Best linear least-squares fits are drawn, depicting the significant growth phases (see the text for details).
Paper: Analyzing the Sequence of Phases Leading to the Formation of the Active Region 13664, with Potential Carrington-like Characteristics
Authors: P. Romano, A. Elmhamdi, A. Marassi, and L. Contarino
Figure caption: Average of the latitudinal (top panel) and longitudinal (bottom panel) components of the horizontal velocities along the latitudinal extension of the AR over time. Positive (white) and negative (black) values correspond to northward and southward directions, respectively, for the latitudinal component. For the longitudinal component, positive (white) and negative (black) values represent westward and eastward directions, respectively. The red box highlights the emergence of the second main bipole. The gray vertical bars indicate periods of SHARP data gaps.
Paper: Extended Shock Breakout and Early Circumstellar Interaction in SN 2024ggi
Authors: Manisha Shrestha, K. Azalee Bostroem, David J. Sand, Griffin Hosseinzadeh, Jennifer E. Andrews, Yize Dong, 一泽 董, Emily Hoang, Daryl Janzen, Jeniveve Pearson, Jacob E. Jencson, M. J. Lundquist, Darshana Mehta, Aravind P. Ravi, Nicolás Meza Retamal, Stefano Valenti, Peter J. Brown, Saurabh W. Jha, Colin Macrie, Brian Hsu, Joseph Farah, D. Andrew Howell, Curtis McCully, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Giacomo Terreran, Lindsey Kwok, Nathan Smith, Michaela Schwab, Aidan Martas, Ricardo R. Munoz, Gustavo E. Medina, Ting S. Li, Paula Diaz, Daichi Hiramatsu, Brad E. Tucker, J. C. Wheeler, Xiaofeng Wang, Qian Zhai, Jujia Zhang, Anjasha Gangopadhyay, Yi Yang, Claudia P. Gutiérrez
Figure caption: Comparison of our +1.27 day spectrum (black) to Boian & Groh (2019) models with L = 1.5 × 109 L ☉ and ﹩\dot{M}=3\times {10}^{-3}\ {M}_{\odot }\ {\mathrm{yr}}^{-1}﹩ for three different abundances. The orange line shows the He-rich abundance representing an LBV/WN/stripped star, the green line is for high-mass RSG/BSG/YSG with CNO-processed abundance, and the red is for solar abundance representing a low-mass RSG. Vertical lines represent the ions that are used as a diagnostic of the progenitor in Boian & Groh (2019). The model spectra have been convolved with a Gaussian kernel to mimic the resolution of the observed spectrum.
Paper: Extended Shock Breakout and Early Circumstellar Interaction in SN 2024ggi
Authors: Manisha Shrestha, K. Azalee Bostroem, David J. Sand, Griffin Hosseinzadeh, Jennifer E. Andrews, Yize Dong, 一泽 董, Emily Hoang, Daryl Janzen, Jeniveve Pearson, Jacob E. Jencson, M. J. Lundquist, Darshana Mehta, Aravind P. Ravi, Nicolás Meza Retamal, Stefano Valenti, Peter J. Brown, Saurabh W. Jha, Colin Macrie, Brian Hsu, Joseph Farah, D. Andrew Howell, Curtis McCully, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Giacomo Terreran, Lindsey Kwok, Nathan Smith, Michaela Schwab, Aidan Martas, Ricardo R. Munoz, Gustavo E. Medina, Ting S. Li, Paula Diaz, Daichi Hiramatsu, Brad E. Tucker, J. C. Wheeler, Xiaofeng Wang, Qian Zhai, Jujia Zhang, Anjasha Gangopadhyay, Yi Yang, Claudia P. Gutiérrez
Figure caption: Extinction-corrected B–V color curve of SN 2024ggi (black) and SN 2023ixf (red) for the first 16 days. The last epoch where the spectra have flash features for both SN 2024ggi (black) and SN 2023ixf (red) are indicated by the shaded regions. The extent of the shaded region is the length of time between the last spectrum showing a flash feature and the first spectrum with no flash features. The data at phases before 2 days show that the color is getting bluer quickly prior to evolving redward. (The data used to create this figure are available in the published article.)
Paper: Extended Shock Breakout and Early Circumstellar Interaction in SN 2024ggi
Authors: Manisha Shrestha, K. Azalee Bostroem, David J. Sand, Griffin Hosseinzadeh, Jennifer E. Andrews, Yize Dong, 一泽 董, Emily Hoang, Daryl Janzen, Jeniveve Pearson, Jacob E. Jencson, M. J. Lundquist, Darshana Mehta, Aravind P. Ravi, Nicolás Meza Retamal, Stefano Valenti, Peter J. Brown, Saurabh W. Jha, Colin Macrie, Brian Hsu, Joseph Farah, D. Andrew Howell, Curtis McCully, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Giacomo Terreran, Lindsey Kwok, Nathan Smith, Michaela Schwab, Aidan Martas, Ricardo R. Munoz, Gustavo E. Medina, Ting S. Li, Paula Diaz, Daichi Hiramatsu, Brad E. Tucker, J. C. Wheeler, Xiaofeng Wang, Qian Zhai, Jujia Zhang, Anjasha Gangopadhyay, Yi Yang, Claudia P. Gutiérrez
Figure caption: Left: high-resolution MIKE data +1.22 days (black) and +1.49 days (red) focusing on the Hα feature. The brown dashed line represents the peak of the feature. We calculate a velocity relative to this wavelength at the position of the shallow absorption feature, a P Cygni signature. The dashed–dotted blue line is placed at the shallow absorption feature at −37 ± 4 km s−1, which we use as one of the markers for CSM velocity. He II is also identified by the yellow dashed line. Right: line profiles of Hα, He II λ4685.5, and C IV from the first epoch (+1.22 days), where the black dashed line represents the rest wavelength of these lines. We see a shift in velocity of −75 km s−1 for all of the lines, shown by the blue dotted line.
Paper: Extended Shock Breakout and Early Circumstellar Interaction in SN 2024ggi
Authors: Manisha Shrestha, K. Azalee Bostroem, David J. Sand, Griffin Hosseinzadeh, Jennifer E. Andrews, Yize Dong, 一泽 董, Emily Hoang, Daryl Janzen, Jeniveve Pearson, Jacob E. Jencson, M. J. Lundquist, Darshana Mehta, Aravind P. Ravi, Nicolás Meza Retamal, Stefano Valenti, Peter J. Brown, Saurabh W. Jha, Colin Macrie, Brian Hsu, Joseph Farah, D. Andrew Howell, Curtis McCully, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Giacomo Terreran, Lindsey Kwok, Nathan Smith, Michaela Schwab, Aidan Martas, Ricardo R. Munoz, Gustavo E. Medina, Ting S. Li, Paula Diaz, Daichi Hiramatsu, Brad E. Tucker, J. C. Wheeler, Xiaofeng Wang, Qian Zhai, Jujia Zhang, Anjasha Gangopadhyay, Yi Yang, Claudia P. Gutiérrez
Figure caption: Comparison of SN 2024ggi spectra (black) with r1w4 model (red) from Dessart et al. (2017). The observational and model epochs are shown in their respective colors on the right. This is the only model that has the N III line, which is present in the observed spectrum. Thus, we present this model as the best representation of the observed spectrum. However, the model spectra evolve faster than the observed spectra of SN 2024ggi. This difference in evolution was also seen for SN 2023ixf (Bostroem et al. 2023).
Paper: Extended Shock Breakout and Early Circumstellar Interaction in SN 2024ggi
Authors: Manisha Shrestha, K. Azalee Bostroem, David J. Sand, Griffin Hosseinzadeh, Jennifer E. Andrews, Yize Dong, 一泽 董, Emily Hoang, Daryl Janzen, Jeniveve Pearson, Jacob E. Jencson, M. J. Lundquist, Darshana Mehta, Aravind P. Ravi, Nicolás Meza Retamal, Stefano Valenti, Peter J. Brown, Saurabh W. Jha, Colin Macrie, Brian Hsu, Joseph Farah, D. Andrew Howell, Curtis McCully, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Giacomo Terreran, Lindsey Kwok, Nathan Smith, Michaela Schwab, Aidan Martas, Ricardo R. Munoz, Gustavo E. Medina, Ting S. Li, Paula Diaz, Daichi Hiramatsu, Brad E. Tucker, J. C. Wheeler, Xiaofeng Wang, Qian Zhai, Jujia Zhang, Anjasha Gangopadhyay, Yi Yang, Claudia P. Gutiérrez
Figure caption: Temperature (red) and photospheric radius (black) evolution of SN 2024ggi derived from fitting a blackbody SED to the multiband photometry.
Paper: Extended Shock Breakout and Early Circumstellar Interaction in SN 2024ggi
Authors: Manisha Shrestha, K. Azalee Bostroem, David J. Sand, Griffin Hosseinzadeh, Jennifer E. Andrews, Yize Dong, 一泽 董, Emily Hoang, Daryl Janzen, Jeniveve Pearson, Jacob E. Jencson, M. J. Lundquist, Darshana Mehta, Aravind P. Ravi, Nicolás Meza Retamal, Stefano Valenti, Peter J. Brown, Saurabh W. Jha, Colin Macrie, Brian Hsu, Joseph Farah, D. Andrew Howell, Curtis McCully, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Giacomo Terreran, Lindsey Kwok, Nathan Smith, Michaela Schwab, Aidan Martas, Ricardo R. Munoz, Gustavo E. Medina, Ting S. Li, Paula Diaz, Daichi Hiramatsu, Brad E. Tucker, J. C. Wheeler, Xiaofeng Wang, Qian Zhai, Jujia Zhang, Anjasha Gangopadhyay, Yi Yang, Claudia P. Gutiérrez
Figure caption: Shock-cooling modeling of SN 2024ggi using the prescription of Morag et al. (2023). The model does a good job fitting the rise after the first day of data to the maximum for all filters and initial plateau for optical filters of SN 2024ggi but does not correctly estimate the explosion time, with SN emission apparent a full day before the model’s preferred explosion epoch. Similar behavior and mismatch to the model were seen in the case of SN 2023ixf (Hosseinzadeh et al. 2023).
Paper: Extended Shock Breakout and Early Circumstellar Interaction in SN 2024ggi
Authors: Manisha Shrestha, K. Azalee Bostroem, David J. Sand, Griffin Hosseinzadeh, Jennifer E. Andrews, Yize Dong, 一泽 董, Emily Hoang, Daryl Janzen, Jeniveve Pearson, Jacob E. Jencson, M. J. Lundquist, Darshana Mehta, Aravind P. Ravi, Nicolás Meza Retamal, Stefano Valenti, Peter J. Brown, Saurabh W. Jha, Colin Macrie, Brian Hsu, Joseph Farah, D. Andrew Howell, Curtis McCully, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Giacomo Terreran, Lindsey Kwok, Nathan Smith, Michaela Schwab, Aidan Martas, Ricardo R. Munoz, Gustavo E. Medina, Ting S. Li, Paula Diaz, Daichi Hiramatsu, Brad E. Tucker, J. C. Wheeler, Xiaofeng Wang, Qian Zhai, Jujia Zhang, Anjasha Gangopadhyay, Yi Yang, Claudia P. Gutiérrez
Figure caption: The two panels show narrow emission lines identified in high-resolution MIKE data from the first (black; +1.22 days) and second (red; +1.49 days) epochs. The spectra are shifted by −75 km s−1 to clearly indicate the narrow emission lines. In the first panel, there are N III, C III, and He II lines identified by pink, blue, and yellow dashed lines, respectively. The second panel zooms in on the C IV lines. The lines evolve rapidly within a few hours between the two epochs.
Paper: Extended Shock Breakout and Early Circumstellar Interaction in SN 2024ggi
Authors: Manisha Shrestha, K. Azalee Bostroem, David J. Sand, Griffin Hosseinzadeh, Jennifer E. Andrews, Yize Dong, 一泽 董, Emily Hoang, Daryl Janzen, Jeniveve Pearson, Jacob E. Jencson, M. J. Lundquist, Darshana Mehta, Aravind P. Ravi, Nicolás Meza Retamal, Stefano Valenti, Peter J. Brown, Saurabh W. Jha, Colin Macrie, Brian Hsu, Joseph Farah, D. Andrew Howell, Curtis McCully, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Giacomo Terreran, Lindsey Kwok, Nathan Smith, Michaela Schwab, Aidan Martas, Ricardo R. Munoz, Gustavo E. Medina, Ting S. Li, Paula Diaz, Daichi Hiramatsu, Brad E. Tucker, J. C. Wheeler, Xiaofeng Wang, Qian Zhai, Jujia Zhang, Anjasha Gangopadhyay, Yi Yang, Claudia P. Gutiérrez
Figure caption: Pseudobolometric light curve of SN 2024ggi for the first ≲1.3 days after the explosion. There is a clear evolution in the slope of the luminosity increase in a short period of time. We fit two different power laws to the data set. The very early data are best fit by a power-law index of 3.63 and the second set by a power-law index of 4.67. These fits are shown as solid red dashed-dotted and blue dashed lines for each set of data.
Paper: Extended Shock Breakout and Early Circumstellar Interaction in SN 2024ggi
Authors: Manisha Shrestha, K. Azalee Bostroem, David J. Sand, Griffin Hosseinzadeh, Jennifer E. Andrews, Yize Dong, 一泽 董, Emily Hoang, Daryl Janzen, Jeniveve Pearson, Jacob E. Jencson, M. J. Lundquist, Darshana Mehta, Aravind P. Ravi, Nicolás Meza Retamal, Stefano Valenti, Peter J. Brown, Saurabh W. Jha, Colin Macrie, Brian Hsu, Joseph Farah, D. Andrew Howell, Curtis McCully, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Giacomo Terreran, Lindsey Kwok, Nathan Smith, Michaela Schwab, Aidan Martas, Ricardo R. Munoz, Gustavo E. Medina, Ting S. Li, Paula Diaz, Daichi Hiramatsu, Brad E. Tucker, J. C. Wheeler, Xiaofeng Wang, Qian Zhai, Jujia Zhang, Anjasha Gangopadhyay, Yi Yang, Claudia P. Gutiérrez
Figure caption: Pseudobolometric light curve of SN 2024ggi (black) compared to SN 2023ixf (red) from Hosseinzadeh et al. (2023), excluding data from amateur astronomers for the first +2.5 days after the explosion. The rise in luminosity for SN 2024ggi is faster than the rise observed for SN 2023ixf.
Paper: Extended Shock Breakout and Early Circumstellar Interaction in SN 2024ggi
Authors: Manisha Shrestha, K. Azalee Bostroem, David J. Sand, Griffin Hosseinzadeh, Jennifer E. Andrews, Yize Dong, 一泽 董, Emily Hoang, Daryl Janzen, Jeniveve Pearson, Jacob E. Jencson, M. J. Lundquist, Darshana Mehta, Aravind P. Ravi, Nicolás Meza Retamal, Stefano Valenti, Peter J. Brown, Saurabh W. Jha, Colin Macrie, Brian Hsu, Joseph Farah, D. Andrew Howell, Curtis McCully, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Giacomo Terreran, Lindsey Kwok, Nathan Smith, Michaela Schwab, Aidan Martas, Ricardo R. Munoz, Gustavo E. Medina, Ting S. Li, Paula Diaz, Daichi Hiramatsu, Brad E. Tucker, J. C. Wheeler, Xiaofeng Wang, Qian Zhai, Jujia Zhang, Anjasha Gangopadhyay, Yi Yang, Claudia P. Gutiérrez
Figure caption: Optical spectral comparison of SN 2024ggi (black) and SN 2023ixf (red) for the first ∼4.5 days after explosion. Interesting lines are identified, and the epoch for each panel is shown for the two SNe. The first epoch of SN 2023ixf is several hours later than SN 2024ggi, where the He II line is still developing. Most of the lines are present for both the SNe. However, the strength of the lines rapidly declines for SN 2024ggi, with almost all the flash features vanishing by day 3.5, whereas the SN 2023ixf lines decline more slowly and are present even at +5.3 days. This difference can point to the CSM around SN 2024ggi being more confined than the CSM around SN 2023ixf.
Paper: First Direct Evidence for Keplerian Rotation in Quasar Inner Broad-line Regions
Authors: C. Fian, J. Jiménez-Vicente, E. Mediavilla, J. A. Muñoz, D. Chelouche, S. Kaspi, R. Forés-Toribio
Figure caption: Kinematic responses to microlensing for SDSS J1004+4112 and SDSS J1206+4332. The left panels show the average C IV and Si IV line profiles for images A (black) and B (gray). The middle panels illustrate the magnitude differences between the images in the line wings. The rightmost panels display the estimated sizes of different kinematic regions as a function of velocity, along with a Keplerian fit (dashed black line). Upper size limits are shown as triangles and are excluded from the Keplerian fit.
Paper: First Direct Evidence for Keplerian Rotation in Quasar Inner Broad-line Regions
Authors: C. Fian, J. Jiménez-Vicente, E. Mediavilla, J. A. Muñoz, D. Chelouche, S. Kaspi, R. Forés-Toribio
Figure caption: Composite velocity–size curve (black data points), along with a Keplerian fit (dashed black line). The gray-shaded area represents the 1σ uncertainty interval of the Keplerian fit. The velocity curves for individual systems and/or emission lines are represented by blue and red data points, which correspond to the blue and red wings, respectively. Upper size limits are shown as triangles and are excluded from the Keplerian fit.
Paper: First Direct Evidence for Keplerian Rotation in Quasar Inner Broad-line Regions
Authors: C. Fian, J. Jiménez-Vicente, E. Mediavilla, J. A. Muñoz, D. Chelouche, S. Kaspi, R. Forés-Toribio
Figure caption: Same as Figure 1, but focusing on the red line wings of the systems SDSS J1001+5027, HE 1104−1805, and SDSS J1339+1310. For HE 1104−1805 and SDSS J1339+1310, the middle and rightmost panels show the results for both the C IV and Si IV lines.
Paper: In LIGO’s Sight? Vigorous Coherent Gravitational Waves from Cooled Collapsar Disks
Authors: Ore Gottlieb, Amir Levinson, Yuri Levin
Figure caption: 3D renderings illustrate the logarithmic mass density (in cgs) of collapsar accretion disks. The length scale can be measured with respect to the BH event horizon radius, represented by a black circle. (a) The early formation stages of the disk (≈1 s) feature low-density spiral density waves. (b) At t ≳ 1 s, with the accumulation of infalling gas, a high-density ring forms at R ≈ 15r  g . RWIs in the disk give rise to nonaxisymmetric modes (shown at t ≈ 5 s). Over time, the disk viscously spreads and its density progressively drops. (c) In the absence of strong cooling, the disk exhibits an extended structure (note that the horizon size in panels (a) and (b) is considerably larger than that in panel (c)) and attains lower densities compared to strongly cooled disks. Consequently, weakly cooled disks exhibit spiral arms at all times (shown at t ≈ 2 s), giving rise to a weaker GW signal. Full movies showcasing the evolution of all collapsar accretion disks are available at http://www.oregottlieb.com/disk_gw.html and on Zenodo (doi:10.5281/zenodo.13139529).
Paper: In LIGO’s Sight? Vigorous Coherent Gravitational Waves from Cooled Collapsar Disks
Authors: Ore Gottlieb, Amir Levinson, Yuri Levin
Figure caption: Top: edge-on (red) and face-on (blue) spectra for models C (first column from left), Ca (second column), Cb (third column), and Cc (fourth column) are presented, with different rows depicting the spectra at various times. The black lines represent the sensitivity of various GW detectors. During the disk formation stage (first row), all models exhibit a quasi-flat spectrum. When cooling is strong (first three columns), Rossby vortices develop, leading to pronounced GW peak frequencies as the disk evolves. A movie showcasing the evolution of the GW spectrum is available at http://www.oregottlieb.com/disk_gw.html or on Zenodo (doi:10.5281/zenodo.13139529). Bottom: the spectrograms for face-on observers over a moving time window of 0.4 s illustrate the signal amplification after ≲1 s. The spectrogram of model Ca resembles that of C.
Paper: In LIGO’s Sight? Vigorous Coherent Gravitational Waves from Cooled Collapsar Disks
Authors: Ore Gottlieb, Amir Levinson, Yuri Levin
Figure caption: (a) The mass density in logarithmic scale map of model C at t = 3.4 s with velocity streamlines in the corotating frame of the high-density wave at (x, y) ≈ (–150, 100) km portray a trapped Rossby vortex. (b) The mass accretion rate on the BH horizon remains roughly constant in time and across models. (c) The jet efficiency on the BH horizon is substantial for rapidly spinning BHs with strong magnetic fields.