adsabs/AstroCLIMB huggingface dataset:
Paper: XRISM Forecast for the Coma Cluster: Stormy, with a Steep Power Spectrum
Authors: Marc Audard, Hisamitsu Awaki, Ralf Ballhausen, Aya Bamba, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Gregory V. Brown, Lia Corrales, Elisa Costantini, Renata Cumbee, Maria Diaz Trigo, Chris Done, Tadayasu Dotani, Ken Ebisawa, Megan E. Eckart, Dominique Eckert, Satoshi Eguchi, Teruaki Enoto, Yuichiro Ezoe, Adam Foster, Ryuichi Fujimoto, Yutaka Fujita, Yasushi Fukazawa, Kotaro Fukushima, Akihiro Furuzawa, Luigi Gallo, Javier A. García, Liyi Gu, Matteo Guainazzi, Kouichi Hagino, Kenji Hamaguchi, Isamu Hatsukade, Katsuhiro Hayashi, Takayuki Hayashi, Natalie Hell, Edmund Hodges-Kluck, Ann Hornschemeier, Yuto Ichinohe, Daiki Ishi, Manabu Ishida, Kumi Ishikawa, Yoshitaka Ishisaki, Jelle Kaastra, Timothy Kallman, Erin Kara, Satoru Katsuda, Yoshiaki Kanemaru, Richard Kelley, Caroline Kilbourne, Shunji Kitamoto, Shogo Kobayashi, Takayoshi Kohmura, Aya Kubota, Maurice Leutenegger, Michael Loewenstein, Yoshitomo Maeda, Maxim Markevitch, Hironori Matsumoto, Kyoko Matsushita, Dan McCammon, Brian McNamara, François Mernier, Eric D. Miller, Jon M. Miller, Ikuyuki Mitsuishi, Misaki Mizumoto, Tsunefumi Mizuno, Koji Mori, Koji Mukai, Hiroshi Murakami, Richard Mushotzky, Hiroshi Nakajima, Kazuhiro Nakazawa, Jan-Uwe Ness, Kumiko Nobukawa, Masayoshi Nobukawa, Hirofumi Noda, Hirokazu Odaka, Shoji Ogawa, Anna Ogorzałek, Takashi Okajima, Naomi Ota, Stéphane Paltani, Robert Petre, Paul Plucinsky, Frederick S. Porter, Katja Pottschmidt, Kosuke Sato, Toshiki Sato, Makoto Sawada, Hiromi Seta, Megumi Shidatsu, Aurora Simionescu, Randall Smith, Hiromasa Suzuki, Andrew Szymkowiak, Hiromitsu Takahashi, Mai Takeo, Toru Tamagawa, Keisuke Tamura, Takaaki Tanaka, Atsushi Tanimoto, Makoto Tashiro, Yukikatsu Terada, Yuichi Terashima, Yohko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi Tsuru, Ayşegül Tümer, Hiroyuki Uchida, Nagomi Uchida, Yuusuke Uchida, Hideki Uchiyama, Shutaro Ueda, Yoshihiro Ueda, Shinichiro Uno, Jacco Vink, Shin Watanabe, Brian J. Williams, Satoshi Yamada, Shinya Yamada, Hiroya Yamaguchi, Kazutaka Yamaoka, Noriko Yamasaki, Makoto Yamauchi, Shigeo Yamauchi, Tahir Yaqoob, Tomokage Yoneyama, Tessei Yoshida, Mihoko Yukita, Irina Zhuravleva, Andrew Fabian, Dylan Nelson, Nobuhiro Okabe, Annalisa Pillepich, Cicely Potter, Manon Regamey, Kosei Sakai, Mona Shishido, Nhut Truong, Daniel R. Wik, John ZuHone
Figure caption: XRISM Resolve spectra for (a) Center and (b) South pointings in the He-like and H-like Fe line region, binned by 4 and 8 eV, respectively. Red lines show the best-fit models (Table 1), while the light-blue line represents a model with the cluster optical redshift; a shift is evident.
Paper: XRISM Forecast for the Coma Cluster: Stormy, with a Steep Power Spectrum
Authors: Marc Audard, Hisamitsu Awaki, Ralf Ballhausen, Aya Bamba, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Gregory V. Brown, Lia Corrales, Elisa Costantini, Renata Cumbee, Maria Diaz Trigo, Chris Done, Tadayasu Dotani, Ken Ebisawa, Megan E. Eckart, Dominique Eckert, Satoshi Eguchi, Teruaki Enoto, Yuichiro Ezoe, Adam Foster, Ryuichi Fujimoto, Yutaka Fujita, Yasushi Fukazawa, Kotaro Fukushima, Akihiro Furuzawa, Luigi Gallo, Javier A. García, Liyi Gu, Matteo Guainazzi, Kouichi Hagino, Kenji Hamaguchi, Isamu Hatsukade, Katsuhiro Hayashi, Takayuki Hayashi, Natalie Hell, Edmund Hodges-Kluck, Ann Hornschemeier, Yuto Ichinohe, Daiki Ishi, Manabu Ishida, Kumi Ishikawa, Yoshitaka Ishisaki, Jelle Kaastra, Timothy Kallman, Erin Kara, Satoru Katsuda, Yoshiaki Kanemaru, Richard Kelley, Caroline Kilbourne, Shunji Kitamoto, Shogo Kobayashi, Takayoshi Kohmura, Aya Kubota, Maurice Leutenegger, Michael Loewenstein, Yoshitomo Maeda, Maxim Markevitch, Hironori Matsumoto, Kyoko Matsushita, Dan McCammon, Brian McNamara, François Mernier, Eric D. Miller, Jon M. Miller, Ikuyuki Mitsuishi, Misaki Mizumoto, Tsunefumi Mizuno, Koji Mori, Koji Mukai, Hiroshi Murakami, Richard Mushotzky, Hiroshi Nakajima, Kazuhiro Nakazawa, Jan-Uwe Ness, Kumiko Nobukawa, Masayoshi Nobukawa, Hirofumi Noda, Hirokazu Odaka, Shoji Ogawa, Anna Ogorzałek, Takashi Okajima, Naomi Ota, Stéphane Paltani, Robert Petre, Paul Plucinsky, Frederick S. Porter, Katja Pottschmidt, Kosuke Sato, Toshiki Sato, Makoto Sawada, Hiromi Seta, Megumi Shidatsu, Aurora Simionescu, Randall Smith, Hiromasa Suzuki, Andrew Szymkowiak, Hiromitsu Takahashi, Mai Takeo, Toru Tamagawa, Keisuke Tamura, Takaaki Tanaka, Atsushi Tanimoto, Makoto Tashiro, Yukikatsu Terada, Yuichi Terashima, Yohko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi Tsuru, Ayşegül Tümer, Hiroyuki Uchida, Nagomi Uchida, Yuusuke Uchida, Hideki Uchiyama, Shutaro Ueda, Yoshihiro Ueda, Shinichiro Uno, Jacco Vink, Shin Watanabe, Brian J. Williams, Satoshi Yamada, Shinya Yamada, Hiroya Yamaguchi, Kazutaka Yamaoka, Noriko Yamasaki, Makoto Yamauchi, Shigeo Yamauchi, Tahir Yaqoob, Tomokage Yoneyama, Tessei Yoshida, Mihoko Yukita, Irina Zhuravleva, Andrew Fabian, Dylan Nelson, Nobuhiro Okabe, Annalisa Pillepich, Cicely Potter, Manon Regamey, Kosei Sakai, Mona Shishido, Nhut Truong, Daniel R. Wik, John ZuHone
Figure caption: The spectrum from the NE quadrant of the Center field around the Fe Lyα line, binned by 4 eV. The red line shows a BAPEC model fit in the interval shown in Figure 2 (including Fe Heα and Lyα lines). An excess is observed in the Lyα2 component. The blue line shows a fit with additional flux in this line, required at ∼3σ significance.
Paper: XRISM Forecast for the Coma Cluster: Stormy, with a Steep Power Spectrum
Authors: Marc Audard, Hisamitsu Awaki, Ralf Ballhausen, Aya Bamba, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Gregory V. Brown, Lia Corrales, Elisa Costantini, Renata Cumbee, Maria Diaz Trigo, Chris Done, Tadayasu Dotani, Ken Ebisawa, Megan E. Eckart, Dominique Eckert, Satoshi Eguchi, Teruaki Enoto, Yuichiro Ezoe, Adam Foster, Ryuichi Fujimoto, Yutaka Fujita, Yasushi Fukazawa, Kotaro Fukushima, Akihiro Furuzawa, Luigi Gallo, Javier A. García, Liyi Gu, Matteo Guainazzi, Kouichi Hagino, Kenji Hamaguchi, Isamu Hatsukade, Katsuhiro Hayashi, Takayuki Hayashi, Natalie Hell, Edmund Hodges-Kluck, Ann Hornschemeier, Yuto Ichinohe, Daiki Ishi, Manabu Ishida, Kumi Ishikawa, Yoshitaka Ishisaki, Jelle Kaastra, Timothy Kallman, Erin Kara, Satoru Katsuda, Yoshiaki Kanemaru, Richard Kelley, Caroline Kilbourne, Shunji Kitamoto, Shogo Kobayashi, Takayoshi Kohmura, Aya Kubota, Maurice Leutenegger, Michael Loewenstein, Yoshitomo Maeda, Maxim Markevitch, Hironori Matsumoto, Kyoko Matsushita, Dan McCammon, Brian McNamara, François Mernier, Eric D. Miller, Jon M. Miller, Ikuyuki Mitsuishi, Misaki Mizumoto, Tsunefumi Mizuno, Koji Mori, Koji Mukai, Hiroshi Murakami, Richard Mushotzky, Hiroshi Nakajima, Kazuhiro Nakazawa, Jan-Uwe Ness, Kumiko Nobukawa, Masayoshi Nobukawa, Hirofumi Noda, Hirokazu Odaka, Shoji Ogawa, Anna Ogorzałek, Takashi Okajima, Naomi Ota, Stéphane Paltani, Robert Petre, Paul Plucinsky, Frederick S. Porter, Katja Pottschmidt, Kosuke Sato, Toshiki Sato, Makoto Sawada, Hiromi Seta, Megumi Shidatsu, Aurora Simionescu, Randall Smith, Hiromasa Suzuki, Andrew Szymkowiak, Hiromitsu Takahashi, Mai Takeo, Toru Tamagawa, Keisuke Tamura, Takaaki Tanaka, Atsushi Tanimoto, Makoto Tashiro, Yukikatsu Terada, Yuichi Terashima, Yohko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi Tsuru, Ayşegül Tümer, Hiroyuki Uchida, Nagomi Uchida, Yuusuke Uchida, Hideki Uchiyama, Shutaro Ueda, Yoshihiro Ueda, Shinichiro Uno, Jacco Vink, Shin Watanabe, Brian J. Williams, Satoshi Yamada, Shinya Yamada, Hiroya Yamaguchi, Kazutaka Yamaoka, Noriko Yamasaki, Makoto Yamauchi, Shigeo Yamauchi, Tahir Yaqoob, Tomokage Yoneyama, Tessei Yoshida, Mihoko Yukita, Irina Zhuravleva, Andrew Fabian, Dylan Nelson, Nobuhiro Okabe, Annalisa Pillepich, Cicely Potter, Manon Regamey, Kosei Sakai, Mona Shishido, Nhut Truong, Daniel R. Wik, John ZuHone
Figure caption: XRISM Resolve FOVs and exposure times overlaid on the XMM-Newton image of the Coma Cluster (J. S. Sanders et al. 2020). The two BCGs are marked.
Paper: Starspot Area Coverage: Correlation with Age and Spectral Type in FGK and M Stars
Authors: Alexandre Araújo, Ciria Lima, Fabian Menezes, Adriana Valio
Figure caption: Left panel: synthesized 2D image of the star with a gray spot, while the black circle depicts the transiting planet. Middle top panel: light-curve transit (black dots) with the spot signature at about 1 hr from midtransit. The red curve depicts the model without spots. Middle bottom panel: residuals of the observed light curve after the spotless model subtraction. The large peak seen in residuals is understood as the starspots. Right panel: fraction of stellar surface area covered by the spots for all the transits in CoRoT-2.
Paper: Starspot Area Coverage: Correlation with Age and Spectral Type in FGK and M Stars
Authors: Alexandre Araújo, Ciria Lima, Fabian Menezes, Adriana Valio
Figure caption: Results of the 1000 simulations of the spot area coverage estimated from transit mapping (purple curve) and the “true” total area covered by spots (red curve), for three cases of maximum latitude for the spot’s distribution (40∘, 60∘, and 90∘).
Paper: Starspot Area Coverage: Correlation with Age and Spectral Type in FGK and M Stars
Authors: Alexandre Araújo, Ciria Lima, Fabian Menezes, Adriana Valio
Figure caption: Left panel: strong anticorrelation of the percentage of starspot area coverage as a function of stellar age. Middle panel: weak anticorrelation between starspot area coverage (%) and stellar effective temperature. Right panel: moderate correlation between the absolute starspot area coverage and stellar effective temperature.
Paper: Starspot Area Coverage: Correlation with Age and Spectral Type in FGK and M Stars
Authors: Alexandre Araújo, Ciria Lima, Fabian Menezes, Adriana Valio
Figure caption: Left: one simulation of a star with 50 randomly distributed spots. Right: area of the star occulted by the planet with a transit at a latitude of 20∘.
Paper: Starspot Area Coverage: Correlation with Age and Spectral Type in FGK and M Stars
Authors: Alexandre Araújo, Ciria Lima, Fabian Menezes, Adriana Valio
Figure caption: Left panel: weak correlation between stellar ages and the average stellar rotation periods. The green dotted line represents Skumanich’s law for comparison. Right panel: weak anticorrelation of the area coverage of starspots with the mean stellar rotation period.
Paper: Starspot Area Coverage: Correlation with Age and Spectral Type in FGK and M Stars
Authors: Alexandre Araújo, Ciria Lima, Fabian Menezes, Adriana Valio
Figure caption: Average starspot area coverage for different spectral types.
Paper: XRISM Reveals a Remnant Torus in the Low-luminosity AGN M81*
Authors: Jon M. Miller, Ehud Behar, Hisamitsu Awaki, Ann Hornschemeier, Jesse Bluem, Luigi Gallo, Shogo B. Kobayashi, Richard Mushotzky, Masanori Ohno, Robert Petre, Kosuke Sato, Yuichi Terashima, Mihoko Yukita
Figure caption: The Resolve spectrum of M81. The data are binned using the “optimal” algorithm, and then by an extra factor of 2.0 except close to the Fe Kα line. Here the ionized emission lines were fit in SPEX using the “pion” photoionization model. Two zones of photoionized emission are required to fully describe the Fe XXV and Fe XXVI line complexes. The contribution of the less ionized zone is shown in purple, while the more highly ionized and redshifted zone is shown in cyan. Note that the statistical significance of the higher-ionization, redshifted zone is marginal. Please see Sections 3.2 and 3.3 and Table 2 for details.
Paper: XRISM Reveals a Remnant Torus in the Low-luminosity AGN M81*
Authors: Jon M. Miller, Ehud Behar, Hisamitsu Awaki, Ann Hornschemeier, Jesse Bluem, Luigi Gallo, Shogo B. Kobayashi, Richard Mushotzky, Masanori Ohno, Robert Petre, Kosuke Sato, Yuichi Terashima, Mihoko Yukita
Figure caption: The Resolve spectrum of M81. The data are binned using the “optimal” algorithm and then by an extra factor of 2.0 except close to the Fe Kα line. Here the ionized emission lines were fit in SPEX using the “CIE” collisional ionization model. Two zones of collisional emission are required to fully describe the Fe XXV and Fe XXVI line complexes. The contribution from the lower-temperature zone is shown in purple, while the contribution from the hotter zone is shown in cyan. Note that the statistical significance of the higher-temperature, redshifted zone is marginal. Please see Sections 3.2 and 3.4 and Table 3 for details.
Paper: XRISM Reveals a Remnant Torus in the Low-luminosity AGN M81*
Authors: Jon M. Miller, Ehud Behar, Hisamitsu Awaki, Ann Hornschemeier, Jesse Bluem, Luigi Gallo, Shogo B. Kobayashi, Richard Mushotzky, Masanori Ohno, Robert Petre, Kosuke Sato, Yuichi Terashima, Mihoko Yukita
Figure caption: The Resolve spectrum of M81*. Top: the 1.7–10.7 keV band, binned using the “optimal” algorithm. The fit shows a model consisting of a simple power-law and Gaussian functions in XSPEC (see Section 3.1). The trend in blue shows the predicted NXB. Prominent NXB lines are labeled. The NXB is negligible in the band containing the Fe K emission lines observed from M81*. Bottom: the same spectrum and model, shown on a smaller passband and on a linear scale. Laboratory energies for lines observed from M81* are shown in blue. Both neutral Fe Kα,1 and Fe Kα,2 lines are clearly detected, as well as the He-like Fe XXV and H-like Fe XXVI complexes. Please see Section 3.1 and Table 1 for details.
Paper: Magnetic Reconnection–driven Energization of Protons up to ∼400 keV at the Near-Sun Heliospheric Current Sheet
Authors: M. I. Desai, J. F. Drake, T. Phan, Z. Yin, M. Swisdak, D. J. McComas, S. D. Bale, A. Rahmati, D. Larson, W. H. Matthaeus, M. A. Dayeh, M. J. Starkey, N. E. Raouafi, D. G. Mitchell, C. M. S. Cohen, J. R. Szalay, J. Giacalone, M. E. Hill, E. R. Christian, N. A. Schwadron, R. L. McNutt, O. Malandraki, P. Whittlesey, R. Livi, J. C. Kasper
Figure caption: Overview of energetic proton (D. J. McComas et al. 2016), solar wind electron (P. L. Whittlesey et al. 2020), solar wind ion (R. Livi et al. 2022), and magnetic field (S. D. Bale et al. 2016) observations and approximate PSP trajectory associated with the HCS crossing during E14. Time profiles from 05:30 to 10:30 UT on 2022 December 12 of (a) 2 min omnidirectional averages (over 80 EPI-Lo apertures) of ST proton intensities in three energy ranges between ∼67 and 536 keV; energy spectrograms of ST proton intensities integrated over (b) the antisunward-facing EPI-Lo apertures, defined as those with look directions between 120° and 180° from the Sun–PSP vector, and (c) the sunward-facing apertures with look directions within 0°–60° of the Sun–PSP vector; (d) PADs—where PA is the angle between the particle velocity and the magnetic field vector—of ∼67–570 keV protons transformed into the solar wind frame using the Compton–Getting technique (A. H. Compton & I. A. Getting 1935; F. M. Ipavich 1974; M. Zhang 2005) to eliminate convective anisotropies resulting from the bulk solar wind flow; (e) energy flux spectrogram of 433–527 eV electrons, which constitute the magnetic field–aligned electron beam or strahl originating directly from the solar corona (T. D. Phan et al. 2021); (f) proton density measured by SWEAP/SPAN-Ions (see T. Phan et al. 2024); (g) radial component of the solar wind velocity; and (h) magnetic field magnitude, and its vector components in the Sun-centered RTN coordinate system (radial:red, tangential:blue, and normal:green). The red vertical lines show the ∼3.7 hr duration of the E14 HCS crossing and the four intervals identified at the bottom that are selected for detailed analysis in Figure 2. The blue vertical line denotes the time of the IMF polarity reversal, i.e., when the radial component BR in Figure 1(h) changes sign from negative or inward to positive or outward. (i) A 2D sketch showing the approximate PSP trajectory projected on the plane of reconnection. The blue line along the trajectory depicts time intervals and corresponding regions where PSP observed negative or inward IMF polarity, and the red portion shows time intervals and regions of positive or outward polarity.
Paper: Magnetic Reconnection–driven Energization of Protons up to ∼400 keV at the Near-Sun Heliospheric Current Sheet
Authors: M. I. Desai, J. F. Drake, T. Phan, Z. Yin, M. Swisdak, D. J. McComas, S. D. Bale, A. Rahmati, D. Larson, W. H. Matthaeus, M. A. Dayeh, M. J. Starkey, N. E. Raouafi, D. G. Mitchell, C. M. S. Cohen, J. R. Szalay, J. Giacalone, M. E. Hill, E. R. Christian, N. A. Schwadron, R. L. McNutt, O. Malandraki, P. Whittlesey, R. Livi, J. C. Kasper
Figure caption: Left: time development of flux ropes in a simulation of the E14 HCS reconnection event. From top (a) to bottom (e), current sheet evolution at five times, t/τA = 0, 4, 8, 12, and 16, where τA = L0/CA0 is the Alfvén transit time across the simulation domain from kglobal simulations with an ambient guide field of 0.2 times the upstream magnetic field. The color bar indicates the plasma density normalized to 1500 cm−3. The black lines are the in-plane magnetic field. Early time is defined as t/τA = 0, and late time is t/τA = 16. Right: Figures 4(f) and (g), respectively, show the fire-hose parameter ﹩\alpha =1-4\pi \left({P}_{\parallel }-{P}_{\perp }\right)/{B}^{2}﹩ and the out-of-plane magnetic field Bz late in time from the simulation in Figure 4(e). The color bar represents α and Bz normalized to the upstream magnetic field value. Right: Figure 4(h) shows the differential flux of electrons and protons at early and late times from the simulation of Figures 4(a)–(e).
Paper: Magnetic Reconnection–driven Energization of Protons up to ∼400 keV at the Near-Sun Heliospheric Current Sheet
Authors: M. I. Desai, J. F. Drake, T. Phan, Z. Yin, M. Swisdak, D. J. McComas, S. D. Bale, A. Rahmati, D. Larson, W. H. Matthaeus, M. A. Dayeh, M. J. Starkey, N. E. Raouafi, D. G. Mitchell, C. M. S. Cohen, J. R. Szalay, J. Giacalone, M. E. Hill, E. R. Christian, N. A. Schwadron, R. L. McNutt, O. Malandraki, P. Whittlesey, R. Livi, J. C. Kasper
Figure caption: Evolution of PADs during the PSP E14 HCS crossing. (a) High-resolution (10 s) omnidirectional averages of the intensities and (b) SW frame PADs of ∼67–570 keV protons; (c) magnetic field magnitude and vector components from 06:15 to 07:00 UT on 2022 December 12. (d)–(g) Color-coded normalized differential intensities plotted as a function of energy vs. PA during Periods 1–4 identified in Figures 1 and 2(a)–(c). During each period, the intensity in each energy bin is normalized to the maximum intensity observed at that energy. The lack of measurements at ∼155°–180° PAs during Periods 1–3 is due to the relatively sparse or complete lack of coverage of these PAs by EPI-Lo.
Paper: Magnetic Reconnection–driven Energization of Protons up to ∼400 keV at the Near-Sun Heliospheric Current Sheet
Authors: M. I. Desai, J. F. Drake, T. Phan, Z. Yin, M. Swisdak, D. J. McComas, S. D. Bale, A. Rahmati, D. Larson, W. H. Matthaeus, M. A. Dayeh, M. J. Starkey, N. E. Raouafi, D. G. Mitchell, C. M. S. Cohen, J. R. Szalay, J. Giacalone, M. E. Hill, E. R. Christian, N. A. Schwadron, R. L. McNutt, O. Malandraki, P. Whittlesey, R. Livi, J. C. Kasper
Figure caption: Proton differential energy spectrum during the E14 HCS crossing and comparison with kglobal simulations. (a) Differential energy spectrum of ∼200 eV–527 keV protons from 06:20 to 10:00 UT. The solid line shows a power-law fit of the form dJ/dE α E−γ to the proton spectrum between 67 and 527 keV. The spectral index γ along with the measured proton energy range is shown. Note that this proton spectrum exhibits a notably harder or flatter profile and reaches energies nearly 5 times greater than that of the 30–100 keV proton spectrum (with γ values around 8) recorded by PSP in association with fast solar wind microstreams, which may be generated by interchange reconnection processes occurring near the Sun (S. D. Bale et al. 2023). (b) Proton spectra from kglobal simulations (H. Arnold et al. 2019; J. F. Drake et al. 2019; Z. Yin et al. 2024a) of reconnection at the HCS for two representative guide fields of 0.2 and 0.3 of the reconnecting magnetic field. Early and late times in the simulations are described in Figure 4.
Paper: Angle-dependent in Situ Fast Flavor Transformations in Post-neutron-star-merger Disks
Authors: Kelsey A. Lund, Payel Mukhopadhyay, Jonah M. Miller, G. C. McLaughlin
Figure caption: One-zone oscillation problem demonstrating efficacy of our scheme. Central panel shows angular distribution of electron and heavy neutrinos. Right panel shows final configuration, overlaid with the analytic solution. Left panel shows initial and final values of Gν. We initialize a neutrino field with a crossing, and our approach removes the crossing while conserving integrated Gν.
Paper: Angle-dependent in Situ Fast Flavor Transformations in Post-neutron-star-merger Disks
Authors: Kelsey A. Lund, Payel Mukhopadhyay, Jonah M. Miller, G. C. McLaughlin
Figure caption: Same as Figure 6 but where we incorrectly enforce equipartition across all angles of the superzone. In the middle and right panels, we now show all four species. In this procedure, the crossing is fallaciously eliminated by setting Gν = 0 everywhere. The resulting distributions for the four species are significantly distorted.
Paper: Angle-dependent in Situ Fast Flavor Transformations in Post-neutron-star-merger Disks
Authors: Kelsey A. Lund, Payel Mukhopadhyay, Jonah M. Miller, G. C. McLaughlin
Figure caption: Mass distribution of Ye as the ejecta passes through 10 GK. The top two panels show the distribution of Ye as a function of latitude, with zero representing the plane of the disk. The bottom panel shows the fractional mass distribution for the simulation with (pink) and without (teal) oscillations. The outflow in the simulation with FFCs shifts to lower Ye, especially at higher latitudes, indicating enhanced neutron richness in the ejecta.
Paper: Angle-dependent in Situ Fast Flavor Transformations in Post-neutron-star-merger Disks
Authors: Kelsey A. Lund, Payel Mukhopadhyay, Jonah M. Miller, G. C. McLaughlin
Figure caption: Gν recorded at 11 ms, as a function of the angle μ1, representing the projection of the neutrino wavevector ﹩{\boldsymbol{k}}﹩ onto the radial unit vector ﹩\hat{r}﹩, as described in Equation (A1). Results for two simulations with (pink) and without (teal) oscillations are shown. The radial and polar angle coordinates corresponding to each location are indicated in the top-left corner of each panel (see Figure 2). FFCs erase ELN–XLN crossings by eliminating the shallower side of the crossing (smaller integral) while conserving the energy-integrated Gν, consistent with expectations.
Paper: Angle-dependent in Situ Fast Flavor Transformations in Post-neutron-star-merger Disks
Authors: Kelsey A. Lund, Payel Mukhopadhyay, Jonah M. Miller, G. C. McLaughlin
Figure caption: Temperature snapshot at 25 ms including a side view (top) and top-down view (bottom). In each case, the simulation with no oscillations is shown on the left, while the simulation with oscillations is shown on the right. FFCs result in a cooler disk, consistent with enhanced neutrino cooling and suppressed thermal wind.
Paper: Angle-dependent in Situ Fast Flavor Transformations in Post-neutron-star-merger Disks
Authors: Kelsey A. Lund, Payel Mukhopadhyay, Jonah M. Miller, G. C. McLaughlin
Figure caption: Top: total mass of each element produced, as a function of mass number. Bottom: mass-weighted relative abundances of each element produced, with solar abundances shown as gray diamonds. In each case, we plot both the yields from the outflows with (pink) and without (teal) oscillations. We show the results considering all ejecta (solid lines) as well as nonequatorial ejecta (dashed), as described in Section 3.