adsabs/AstroCLIMB huggingface dataset:
Paper: Comprehensive Analysis of the Neutrino Process in Core-collapsing Supernovae
Authors: Heamin Ko, Dukjae Jang, Myung-Ki Cheoun, Motohiko Kusakabe, Hirokazu Sasaki, Xingqun Yao, Toshitaka Kajino, Takehito Hayakawa, Masaomi Ono, Toshihiko Kawano, Grant J. Mathews
Figure caption: (a) The ν–ν interaction diagrams. The left and right diagrams correspond to the diagonal and exchange terms, respectively. (b) The mean-field approximation for the four-fermion interaction of the diagonal and exchange terms in panel (a).
Paper: Comprehensive Analysis of the Neutrino Process in Core-collapsing Supernovae
Authors: Heamin Ko, Dukjae Jang, Myung-Ki Cheoun, Motohiko Kusakabe, Hirokazu Sasaki, Xingqun Yao, Toshitaka Kajino, Takehito Hayakawa, Masaomi Ono, Toshihiko Kawano, Grant J. Mathews
Figure caption: The neutrino spectra including neutrino SI at t = 50, 100, 200, 300, and 500 ms for the NH case. The dashed and solid lines denote the spectra at r = 10 km and 2000 km, respectively. The red, green, and black lines denote ν  e , ν  μ , and ν  τ .
Paper: Comprehensive Analysis of the Neutrino Process in Core-collapsing Supernovae
Authors: Heamin Ko, Dukjae Jang, Myung-Ki Cheoun, Motohiko Kusakabe, Hirokazu Sasaki, Xingqun Yao, Toshitaka Kajino, Takehito Hayakawa, Masaomi Ono, Toshihiko Kawano, Grant J. Mathews
Figure caption: Flavor change probability for ν  e  with neutrino energy E  ν  = 15  MeV, calculated at t = 0. The left and right panels adopt the HKC18 (Blinnikov et al. 2000) and KCK19 (Kusakabe et al. 2019) hydrodynamics models, respectively. The upper and lower panels correspond to the NH and IH, respectively.
Paper: Comprehensive Analysis of the Neutrino Process in Core-collapsing Supernovae
Authors: Heamin Ko, Dukjae Jang, Myung-Ki Cheoun, Motohiko Kusakabe, Hirokazu Sasaki, Xingqun Yao, Toshitaka Kajino, Takehito Hayakawa, Masaomi Ono, Toshihiko Kawano, Grant J. Mathews
Figure caption: The flavor change probabilities, including the shock propagation effect, in the KCK19 model (Kusakabe et al. 2019) at t = 2, 3, 5, and 7 s for E  ν  = 15  MeV. The labels denote the probabilities as in Figure 4, i.e., Pee = P﹩{}_{{\nu }_{e}\to {\nu }_{e}}﹩ and Pxe = P﹩{}_{{\nu }_{\mu }\to {\nu }_{e}}﹩ +P﹩{}_{{\nu }_{\tau }\to {\nu }_{e}}﹩. The left and right panels correspond to the NH and IH, respectively.
Paper: Comprehensive Analysis of the Neutrino Process in Core-collapsing Supernovae
Authors: Heamin Ko, Dukjae Jang, Myung-Ki Cheoun, Motohiko Kusakabe, Hirokazu Sasaki, Xingqun Yao, Toshitaka Kajino, Takehito Hayakawa, Masaomi Ono, Toshihiko Kawano, Grant J. Mathews
Figure caption: The neutrino luminosities for each flavor: ﹩{\nu }_{e},\,{\bar{\nu }}_{e}﹩, and ﹩{\nu }_{x}(=\,{\nu }_{\mu },{\nu }_{\tau },{\bar{\nu }}_{\mu }﹩ and ﹩{\bar{\nu }}_{\tau }﹩) in the region of M  r  ∼ 1.6M ⊙ (corresponding to r ≈ 2300 km). The inset shows an enlarged figure of the x- and y-axes. The yellow line denotes the luminosity calculated by Equation (14) and the others are adopted from Table 2.
Paper: Comprehensive Analysis of the Neutrino Process in Core-collapsing Supernovae
Authors: Heamin Ko, Dukjae Jang, Myung-Ki Cheoun, Motohiko Kusakabe, Hirokazu Sasaki, Xingqun Yao, Toshitaka Kajino, Takehito Hayakawa, Masaomi Ono, Toshihiko Kawano, Grant J. Mathews
Figure caption: The neutrino spectra ﹩(\equiv 4\pi {r}^{2}{\phi }^{{\prime} })﹩ with SI effects for IH. The upper and lower panels show the ν and ﹩\bar{\nu }﹩ cases, respectively.
Paper: Comprehensive Analysis of the Neutrino Process in Core-collapsing Supernovae
Authors: Heamin Ko, Dukjae Jang, Myung-Ki Cheoun, Motohiko Kusakabe, Hirokazu Sasaki, Xingqun Yao, Toshitaka Kajino, Takehito Hayakawa, Masaomi Ono, Toshihiko Kawano, Grant J. Mathews
Figure caption: The number density of electrons and electro-neutrinos. Each dashed line stands for the number density at the post-bounce times t  pb  = 0.05, 0.1, 0.2, 0.3, and 0.5 s, as labeled.
Paper: Comprehensive Analysis of the Neutrino Process in Core-collapsing Supernovae
Authors: Heamin Ko, Dukjae Jang, Myung-Ki Cheoun, Motohiko Kusakabe, Hirokazu Sasaki, Xingqun Yao, Toshitaka Kajino, Takehito Hayakawa, Masaomi Ono, Toshihiko Kawano, Grant J. Mathews
Figure caption: The eigenvalues of the matter states according to the electron number density per N  A  for E  ν  = 15  MeV. The upper and lower panels show the results calculated in the NH and IH schemes, respectively.
Paper: Comprehensive Analysis of the Neutrino Process in Core-collapsing Supernovae
Authors: Heamin Ko, Dukjae Jang, Myung-Ki Cheoun, Motohiko Kusakabe, Hirokazu Sasaki, Xingqun Yao, Toshitaka Kajino, Takehito Hayakawa, Masaomi Ono, Toshihiko Kawano, Grant J. Mathews
Figure caption: Time-evolving radius profiles as a function of the Lagrange mass coordinate. The upper and lower panels show the same models as in Figure 1, respectively.
Paper: Stellar Energetic Particle Transport in the Turbulent and CME-disrupted Stellar Wind of AU Microscopii
Authors: Federico Fraschetti, Julián D. Alvarado-Gómez, Jeremy J. Drake, Ofer Cohen, Cecilia Garraffo
Figure caption: A 3D view of the open (green) and closed (magenta) quiescent stellar wind magnetic field lines. The central sphere is the host star, color coded by the radial component of the local stellar magnetic field on the surface. The transparent gridded sphere marks R = 5 R ⋆. The two circles in the equatorial plane mark the orbits of planet b (solid) and c (dotted) around the star. The colored circular ring at R = R  b  is color coded with the strength of the large-scale magnetic field. The plane B  r  = 0 (where B  r  is the radial component of the magnetic field), that on average corresponds to the CS, is approximately denoted by the purple tilted circle.
Paper: Repeating Ultraluminous X-Ray Bursts and Repeating Fast Radio Bursts: A Possible Association?
Authors: Hao-Yan Chen, Wei-Min Gu, Jin-Bo Fu, Shan-Shan Weng, Junfeng Wang, Mouyuan Sun
Figure caption: The schematic diagram of the NS–WD binary model with an eccentric orbit, where the WD fills its Roche lobe at the periastron. Around the periastron, the mass transfer occurs from the WD to the NS through the inner Lagrange point L 1. Due to the viscous processes, the accreted materials can be fragmented into a number of parts. The system consists of a magnetic WD and an NS with strong dipole magnetic fields. The NS accretion disk is truncated by the magnetic field near the magnetospheric radius R M. Around the magnetospheric radius R M, the accreted material is governed by the magnetic field lines and can leave the disk to approach the NS surface. The magnetic reconnection may be triggered. The strong FRB radiations can be released by the curvature radiation of the electrons (more details can be found in Section 5). Finally, the accreted materials follow the magnetic field lines down to a small area around the polar caps of the NS, forming an accretion column or funnel. The ultraluminous X-ray radiations can be produced from the accretion column. (The sizes of compact objects are not to scale for the purpose of demonstration.)
Paper: Repeating Ultraluminous X-Ray Bursts and Repeating Fast Radio Bursts: A Possible Association?
Authors: Hao-Yan Chen, Wei-Min Gu, Jin-Bo Fu, Shan-Shan Weng, Junfeng Wang, Mouyuan Sun
Figure caption: The relationship between the orbital period P orb and the mass of the central object M 1 for the given eccentricities e and the WD masses M WD. The lines of different colors represent distinct WD masses: 0.02 M ☉ (black), 0.05 M ☉ (blue), and 0.1 M ☉ (red). The solid and dashed lines represent e = 0.95 and 0.99, respectively. The green stars represent three possible orbital periods of the repeating ULXB source in NGC 5128, assuming that M 1 = 1.4 M ☉.
Paper: Repeating Ultraluminous X-Ray Bursts and Repeating Fast Radio Bursts: A Possible Association?
Authors: Hao-Yan Chen, Wei-Min Gu, Jin-Bo Fu, Shan-Shan Weng, Junfeng Wang, Mouyuan Sun
Figure caption: Upper panel: periodogram obtained by folding the arrival time of six ULXBs at all distinguishable trial periods between ∼0.2 and ∼18 days. The folded profiles are evaluated by the length of the longest contiguous phase without any ULXB activity. Three significant trial periods can be found, i.e., P ≃ 0.6428, 2.6485, and 6.0275 days. Lower panel: the activity profiles of the detected ULXBs folded with three trial periods. The phase of zero corresponds to the start time of the first flare minus half a putative period. The histograms of the different colors show the distinct periods, i.e., 0.6428 (blue), 2.6485 (green), and 6.0275 (red) days. It is seen that an activity window exists for the repeating ULXB in NGC 5128.
Paper: Multispacecraft Analysis of the Properties of Magnetohydrodynamic Fluctuations in Sub-Alfvénic Solar Wind Turbulence at 1 au
Authors: S. Q. Zhao, Huirong Yan, Terry Z. Liu, Mingzhe Liu, Huizi Wang
Figure caption: (a) The normalized f rest–k ∥ wavelet power spectra of δ B ⊥1 fluctuations in the rest frame of the solar wind. ﹩{\hat{P}}_{{B}_{\perp 1}}\left({k}_{\parallel },{f}_{\mathrm{rest}}\right)={P}_{{B}_{\perp 1}}({k}_{\parallel },{f}_{\mathrm{rest}})/{P}_{{B}_{\perp 1},\max }({k}_{\parallel },{f}_{\mathrm{rest}})﹩. (b) The normalized theoretical dispersion relation of Alfvén modes. ﹩{\hat{P}}_{{B}_{\perp 1}}\left({k}_{\parallel },{f}_{\mathrm{Alfven}}\right)={P}_{{B}_{\perp 1}}({k}_{\parallel },{f}_{\mathrm{Alfven}})/{P}_{{B}_{\perp 1},\max }({k}_{\parallel },{f}_{\mathrm{Alfven}})﹩. (c) Collision number N vs. k ∥. The horizontal dashed line marks N = 1. (d) The variation of k ⊥ vs. k ∥ for magnetic power of δ B ⊥1 fluctuations (blue curve). The green dashed line represents isotropy: k ∥ = k ⊥. The red dashed line represents the Goldreich–Sridhar scaling ﹩{k}_{\parallel }\propto {k}_{\perp }^{2/3}﹩. These figures use the 30 minute data set of Event 1.
Paper: Multispacecraft Analysis of the Properties of Magnetohydrodynamic Fluctuations in Sub-Alfvénic Solar Wind Turbulence at 1 au
Authors: S. Q. Zhao, Huirong Yan, Terry Z. Liu, Mingzhe Liu, Huizi Wang
Figure caption: (a) Normalized f rest–k ∥ wavelet power spectra of the magnetic field within the ﹩\hat{k}{\hat{b}}_{0}﹩ plane in the rest frame of the solar wind. ﹩{\hat{P}}_{\mathrm{in}\ \hat{k}{\hat{b}}_{0}\ \mathrm{plane}}\left({k}_{\parallel },{f}_{\mathrm{rest}}\right)={P}_{\mathrm{in}\ \hat{k}{\hat{b}}_{0}\ \mathrm{plane}}\left({k}_{\parallel },{f}_{\mathrm{rest}}\right)/{P}_{\mathrm{in}\ \hat{k}{\hat{b}}_{0}\ \mathrm{plane},\max }\left({k}_{\parallel },{f}_{\mathrm{rest}}\right)﹩. (b) The normalized theoretical dispersion relation of fast and slow modes, where ﹩{\hat{P}}_{\mathrm{in}\ \hat{k}{\hat{b}}_{0}\ \mathrm{plane}}\left({k}_{\parallel },{f}_{\mathrm{fast}}\right)={P}_{\mathrm{in}\ \hat{k}{\hat{b}}_{0}\ \mathrm{plane}}({k}_{\parallel },{f}_{\mathrm{fast}})/{P}_{\mathrm{in}\ \hat{k}{\hat{b}}_{0}\ \mathrm{plane},\max }({k}_{\parallel },{f}_{\mathrm{fast}})﹩ and ﹩{\hat{P}}_{\mathrm{in}\ \hat{k}{\hat{b}}_{0}\ \mathrm{plane}}\left({k}_{\parallel },{f}_{\mathrm{slow}}\right)={P}_{\mathrm{in}\ \hat{k}{\hat{b}}_{0}\ \mathrm{plane}}({k}_{\parallel },{f}_{\mathrm{slow}})/{P}_{\mathrm{in}\ \hat{k}{\hat{b}}_{0}\ \mathrm{plane},\max }({k}_{\parallel },{f}_{\mathrm{slow}})﹩. These figures use the 30 minute data set of Event 1.
Paper: Multispacecraft Analysis of the Properties of Magnetohydrodynamic Fluctuations in Sub-Alfvénic Solar Wind Turbulence at 1 au
Authors: S. Q. Zhao, Huirong Yan, Terry Z. Liu, Mingzhe Liu, Huizi Wang
Figure caption: The reduced power spectra of δ B ⊥1 fluctuations using 30 minute data sets. Blue curve ﹩\hat{P}({k}_{\perp })﹩: normalized perpendicular wavenumber spectrum of δ B ⊥1 fluctuations; green curve ﹩\hat{P}({k}_{\parallel })﹩: normalized parallel wavenumber spectrum of δ B ⊥1 fluctuations; black dashed line: power-law fits. (a), (d) Event 1: during 23:00–02:00 UT on 2017 November 23–24. (b), (e) Event 2: during 21:00–23:00 UT on 2017 November 26. (c), (f) Event 3: during 20:15–22:15 UT on 2017 November 14.
Paper: Multispacecraft Analysis of the Properties of Magnetohydrodynamic Fluctuations in Sub-Alfvénic Solar Wind Turbulence at 1 au
Authors: S. Q. Zhao, Huirong Yan, Terry Z. Liu, Mingzhe Liu, Huizi Wang
Figure caption:  k ⊥–k ∥ wavelet power spectra of magnetic field fluctuations within the ﹩\hat{k}{\hat{b}}_{0}﹩ plane using data sets with lengths of 10 minutes (left), 20 minutes (middle), and 30 minutes (right). The magnetic power ﹩{\hat{P}}_{{B}_{\mathrm{in}\ \hat{k}{\hat{b}}_{0}\ \mathrm{plane}}}\left({k}_{\perp },{k}_{\parallel }\right)=({P}_{{B}_{\parallel }}\left({k}_{\perp },{k}_{\parallel }\right)+{P}_{{B}_{\perp 2}}({k}_{\perp },{k}_{\parallel }))/{\left({P}_{{B}_{\parallel }}+{P}_{{B}_{\perp 2}}\right)}_{\max }﹩ is normalized by the maximum power in all bins. (a)–(c) Event 1: during 23:00–02:00 UT on 2017 November 23–24. (d)–(f) Event 2: during 21:00–23:00 UT on 2017 November 26. (g)–(i) Event 3: during 20:15–22:15 UT on 2017 November 14. The purple dashed curves mark k = 0.06/d  i , 0.1/d  i , and 0.2/d  i .
Paper: Multispacecraft Analysis of the Properties of Magnetohydrodynamic Fluctuations in Sub-Alfvénic Solar Wind Turbulence at 1 au
Authors: S. Q. Zhao, Huirong Yan, Terry Z. Liu, Mingzhe Liu, Huizi Wang
Figure caption:  k ⊥–k ∥ wavelet power spectra of magnetic field fluctuations (δ B ⊥1) out of the ﹩\hat{k}{\hat{b}}_{0}﹩ plane using data sets with lengths of 10 minutes (left), 20 minutes (middle), and 30 minutes (right). The magnetic power ﹩{\hat{P}}_{{B}_{\perp 1}}({k}_{\perp },{k}_{\parallel })={P}_{{B}_{\perp 1}}({k}_{\perp },{k}_{\parallel })/{P}_{{B}_{\perp 1},\max }﹩ is normalized by the maximum power in all bins. (a)–(c) Event 1: during 23:00–02:00 UT on 2017 November 23–24. (d)–(f) Event 2: during 21:00–23:00 UT on 2017 November 26. (g)–(i) Event 3: during 20:15–22:15 UT on 2017 November 14. The purple dashed curves mark ﹩k=\sqrt{{k}_{\parallel }^{2}+{k}_{\perp }^{2}}=0.06/{d}_{i}﹩, 0.1/d  i , and 0.2/d  i .
Paper: Multispacecraft Analysis of the Properties of Magnetohydrodynamic Fluctuations in Sub-Alfvénic Solar Wind Turbulence at 1 au
Authors: S. Q. Zhao, Huirong Yan, Terry Z. Liu, Mingzhe Liu, Huizi Wang
Figure caption: Normalized correlation function R(τ)/R(0) vs. timescale τ for magnetic field Z GSE component with window lengths of (a) 10 minutes, (b) 20 minutes, and (c) 30 minutes. The black curves represent R(τ)/R(0) from different moving time windows. The red curves represent average values (s) of R(τ)/R(0) over the corresponding time windows. The yellow shaded regions represent [s − σ, s + σ], where σ is the standard deviation. The horizontal lines mark R(τ)/R(0) = 0.
Paper: Multispacecraft Analysis of the Properties of Magnetohydrodynamic Fluctuations in Sub-Alfvénic Solar Wind Turbulence at 1 au
Authors: S. Q. Zhao, Huirong Yan, Terry Z. Liu, Mingzhe Liu, Huizi Wang
Figure caption: The ratio ﹩\hat{P}({k}_{\perp })﹩/﹩\hat{P}({k}_{\parallel })﹩ of δ B ⊥1 fluctuations. ﹩\hat{P}({k}_{\perp })﹩ represents the normalized perpendicular wavenumber spectrum of δ B ⊥1, and ﹩\hat{P}({k}_{\parallel })﹩ represents the normalized parallel wavenumber spectrum of δ B ⊥1. (a) Event 1: during 23:00–02:00 UT on 2017 November 23–24. (b) Event 2: during 21:00–23:00 UT on 2017 November 26. (c) Event 3: during 20:15–22:15 UT on 2017 November 14.
Paper: Multispacecraft Analysis of the Properties of Magnetohydrodynamic Fluctuations in Sub-Alfvénic Solar Wind Turbulence at 1 au
Authors: S. Q. Zhao, Huirong Yan, Terry Z. Liu, Mingzhe Liu, Huizi Wang
Figure caption: The reduced power spectra of magnetic field fluctuations within the ﹩\hat{k}{\hat{b}}_{0}﹩ plane using 30 minute data sets. Blue curve ﹩\hat{P}({k}_{\perp })﹩: normalized perpendicular wavenumber spectrum; green curve ﹩\hat{P}({k}_{\parallel })﹩: normalized parallel wavenumber spectrum; black dashed lines: power-law fits. (a), (d) Event 1: during 23:00–02:00 UT on 2017 November 23–24. (b), (e) Event 2: during 21:00–23:00 UT on 2017 November 26. (c), (f) Event 3: during 20:15–22:15 UT on 2017 November 14.
Paper: Multispacecraft Analysis of the Properties of Magnetohydrodynamic Fluctuations in Sub-Alfvénic Solar Wind Turbulence at 1 au
Authors: S. Q. Zhao, Huirong Yan, Terry Z. Liu, Mingzhe Liu, Huizi Wang
Figure caption: The ratio ﹩\hat{P}({k}_{\perp })﹩/﹩\hat{P}({k}_{\parallel })﹩ of fluctuations within the ﹩\hat{k}{\hat{b}}_{0}﹩ plane. ﹩\hat{P}({k}_{\perp })﹩ represents the normalized perpendicular wavenumber spectrum, and ﹩\hat{P}({k}_{\parallel })﹩ represents the normalized parallel wavenumber spectrum. (a) Event 1: during 23:00–02:00 UT on 2017 November 23–24. (b) Event 2: during 21:00–23:00 UT on 2017 November 26. (c) Event 3: during 20:15–22:15 UT on 2017 November 14.
Paper: Comprehensive Analysis of the Neutrino Process in Core-collapsing Supernovae
Authors: Heamin Ko, Dukjae Jang, Myung-Ki Cheoun, Motohiko Kusakabe, Hirokazu Sasaki, Xingqun Yao, Toshitaka Kajino, Takehito Hayakawa, Masaomi Ono, Toshihiko Kawano, Grant J. Mathews
Figure caption: The logarithmic nuclear mass fractions in the pre-SN model used in the present work (Kikuchi et al. 2015).
Paper: Comprehensive Analysis of the Neutrino Process in Core-collapsing Supernovae
Authors: Heamin Ko, Dukjae Jang, Myung-Ki Cheoun, Motohiko Kusakabe, Hirokazu Sasaki, Xingqun Yao, Toshitaka Kajino, Takehito Hayakawa, Masaomi Ono, Toshihiko Kawano, Grant J. Mathews
Figure caption: The same as Figure 11, but for the IH case at 10 km and 1000 km.
Paper: Comprehensive Analysis of the Neutrino Process in Core-collapsing Supernovae
Authors: Heamin Ko, Dukjae Jang, Myung-Ki Cheoun, Motohiko Kusakabe, Hirokazu Sasaki, Xingqun Yao, Toshitaka Kajino, Takehito Hayakawa, Masaomi Ono, Toshihiko Kawano, Grant J. Mathews
Figure caption: Logarithmic mass fractions of heavy nuclei: 92Nb, 98Tc, 138La, and 180Ta vs. the mass coordinate. Panels (a) and (b) correspond to the yields for NH and IH, respectively. Panels (c) and (d) denote light nuclei: 7Li, 7Be, 11B, and 11C. The dashed and solid lines, respectively, stand for the results from the hydrodynamics of the HKC18 and KCK19 models. All results are the nuclear abundances synthesized about 50 s following the CCSN explosion.
Paper: Comprehensive Analysis of the Neutrino Process in Core-collapsing Supernovae
Authors: Heamin Ko, Dukjae Jang, Myung-Ki Cheoun, Motohiko Kusakabe, Hirokazu Sasaki, Xingqun Yao, Toshitaka Kajino, Takehito Hayakawa, Masaomi Ono, Toshihiko Kawano, Grant J. Mathews
Figure caption: Logarithmic mass fractions of the heavy and light elements at 50 s after the core bounce over the mass coordinate for the shock effect. Panels (a) and (b) show the heavy elements, while panels (c) and (d) show the light elements. In each panel, the solid and dashed lines denote the cases with and without shock effect, respectively.
Paper: Comprehensive Analysis of the Neutrino Process in Core-collapsing Supernovae
Authors: Heamin Ko, Dukjae Jang, Myung-Ki Cheoun, Motohiko Kusakabe, Hirokazu Sasaki, Xingqun Yao, Toshitaka Kajino, Takehito Hayakawa, Masaomi Ono, Toshihiko Kawano, Grant J. Mathews
Figure caption: Panels (a) and (b) show the mass fractions of the heavy elements as a function of the mass coordinate at 50 s for NH and IH, respectively. Panels (c) and (d) denote the mass fractions of the light elements.
Paper: Comprehensive Analysis of the Neutrino Process in Core-collapsing Supernovae
Authors: Heamin Ko, Dukjae Jang, Myung-Ki Cheoun, Motohiko Kusakabe, Hirokazu Sasaki, Xingqun Yao, Toshitaka Kajino, Takehito Hayakawa, Masaomi Ono, Toshihiko Kawano, Grant J. Mathews
Figure caption: Logarithms of mass fractions of heavy (a) and light (b) elements over the mass coordinate. The solid and dashed lines denote the cases with and without ν-SI, respectively. The dotted line represents the NH case. All results are shown 50 s after the CCSN explosion. The results for the NH case are given without the SI effect.
Paper: Comprehensive Analysis of the Neutrino Process in Core-collapsing Supernovae
Authors: Heamin Ko, Dukjae Jang, Myung-Ki Cheoun, Motohiko Kusakabe, Hirokazu Sasaki, Xingqun Yao, Toshitaka Kajino, Takehito Hayakawa, Masaomi Ono, Toshihiko Kawano, Grant J. Mathews
Figure caption: The main nuclear reactions for 7Li. “Weak” means the channels of the weak interaction, such as beta decays and electron captures. The histograms of some nuclear reactions below a limit are not shown.
Paper: Comprehensive Analysis of the Neutrino Process in Core-collapsing Supernovae
Authors: Heamin Ko, Dukjae Jang, Myung-Ki Cheoun, Motohiko Kusakabe, Hirokazu Sasaki, Xingqun Yao, Toshitaka Kajino, Takehito Hayakawa, Masaomi Ono, Toshihiko Kawano, Grant J. Mathews
Figure caption: Forward (n, γ) reaction rates.
Paper: Comprehensive Analysis of the Neutrino Process in Core-collapsing Supernovae
Authors: Heamin Ko, Dukjae Jang, Myung-Ki Cheoun, Motohiko Kusakabe, Hirokazu Sasaki, Xingqun Yao, Toshitaka Kajino, Takehito Hayakawa, Masaomi Ono, Toshihiko Kawano, Grant J. Mathews
Figure caption: Inverse (γ, n) reaction rates.
Paper: Origin of Nitrogen Isotopic Variations in the Rocky Bodies of the Solar System
Authors: Damanveer S. Grewal
Figure caption: Nitrogen contents and isotopic compositions of CM chondrites as a function of their extent of aqueous alteration (here defined by the alteration scale from Rubin et al. 2007). Both N contents and δ 15N values decrease with increasing extent of aqueous alteration across CM chondrites. Note that the Bells chondrites are not plotted as their Rubin alteration scale index is currently lacking. CM chondrite data is compiled in Table A1 in the Appendix.
Paper: HIFLOW: Generating Diverse HI Maps and Inferring Cosmology while Marginalizing over Astrophysics Using Normalizing Flows
Authors: Sultan Hassan, Francisco Villaescusa-Navarro, Benjamin Wandelt, David N. Spergel, Daniel Anglés-Alcázar, Shy Genel, Miles Cranmer, Greg L. Bryan, Romeel Davé, Rachel S. Somerville, Michael Eickenberg, Desika Narayanan, Shirley Ho, Sambatra Andrianomena
Figure caption: Impact of varying a single CAMELS parameter on the mean pdf over 15 HI maps, sharing the same parameters using the 1P set. As is evidenced by the amount of variation in the mean pdf (μ(pdf)), the HI maps are mostly affected only by the cosmological parameters (Ω m  and σ 8) and not the astrophysical parameters (A﹩{}_{\mathrm{SN}1}﹩, ﹩{{\rm{A}}}_{\mathrm{SN}2}﹩, AAGN1, and AAGN2); hence we choose to condition HIFLOW solely on cosmology.
Paper: HIFLOW: Generating Diverse HI Maps and Inferring Cosmology while Marginalizing over Astrophysics Using Normalizing Flows
Authors: Sultan Hassan, Francisco Villaescusa-Navarro, Benjamin Wandelt, David N. Spergel, Daniel Anglés-Alcázar, Shy Genel, Miles Cranmer, Greg L. Bryan, Romeel Davé, Rachel S. Somerville, Michael Eickenberg, Desika Narayanan, Shirley Ho, Sambatra Andrianomena
Figure caption: Several examples of posterior distributions from HIFLOW for a random set of observed parameters (red cross). The contours represent the 1σ–3σ levels of the posterior. The blue regions of the posterior indicate low probability values, and the lighter blue shows the high probability regions, where the contours reside. At different parts of the prior range, the HIFLOW is able to recover the observed HI maps within 3σ level. By inverting the flow, this is an illustrative example of how HIFLOW can be used to perform efficient and powerful parameter inference.
Paper: HIFLOW: Generating Diverse HI Maps and Inferring Cosmology while Marginalizing over Astrophysics Using Normalizing Flows
Authors: Sultan Hassan, Francisco Villaescusa-Navarro, Benjamin Wandelt, David N. Spergel, Daniel Anglés-Alcázar, Shy Genel, Miles Cranmer, Greg L. Bryan, Romeel Davé, Rachel S. Somerville, Michael Eickenberg, Desika Narayanan, Shirley Ho, Sambatra Andrianomena
Figure caption: Visual summary of the coefficient of determination R 2 between CAMELS and HIFLOW as a function of cosmology for all the testing set (50 simulations). The R 2 values for the average power (μ(P)) and standard deviation power (σ(P)) are shown in the left and right panels, respectively as indicated by subtitles. The R 2 values are higher for μ(P) than σ(P), but nevertheless, in all cases, there is strong correlation between the CAMELS and HIFLOW with R 2 > 90%.