adsabs/AstroCLIMB huggingface dataset:
Paper: High-energy Neutrinos from the Inner Circumnuclear Region of NGC 1068
Authors: Ke Fang, Enrique Lopez Rodriguez, Francis Halzen, John S. Gallagher
Figure caption: Broadband SED of NGC 1068 and its knots C (in dark blue) and S1 (in light blue) in the inner circumnuclear region. The red curve indicates the all-flavor high-energy neutrino emission produced by one knot (assumed to be the same for both knots). The curves (solid for knot C and dashed for knot S1) show the synchrotron and inverse Compton radiation by the accompanying γ-rays and their electromagnetic cascades, respectively. The model parameters in use are R = 0.1 pc and B = 500 mG. The radio to UV measurements of the two knots, from Section 2, are indicated by cross and diamond markers, respectively. The rest of the data points show the multi-messenger emission of NGC 1068. In particular, γ-ray data points and upper limits are from observations of Fermi-LAT, including the Third Fermi-LAT Catolog of High-Energy Sources (Ajello et al. 2017) catalog and Ajello et al. (2023), MAGIC (Acciari et al. 2019), and HAWC (assuming E −3 spectrum; Willox & HAWC Collaboration 2022). The band in X-ray corresponds to the nucleus component of the best-fit model “M2d” of Bauer et al. (2015), which shows the intrinsic, unabsorbed flux of the nucleus at 2–195 keV. The radio, IR, and optical data points are based on observations of NGC 1068 by Mason et al. (2006, 2009), Chhetri et al. (2013), Planck Collaboration et al. (2016), Intema et al. (2017), Doyle et al. (2005), Skrutskie et al. (2006), and Gil de Paz et al. (2007).
Paper: Regulation of Proton–α Differential Flow by Compressive Fluctuations and Ion-scale Instabilities in the Solar Wind
Authors: Xingyu Zhu, Daniel Verscharen, Jiansen He, Bennett A. Maruca, Christopher J. Owen
Figure caption: Comparison of our theoretical predictions for the effective instability thresholds U pα0,crit with observations from Wind. We show the comparison for six different β ∥p0 values. The color-coding represents the binned PDFs of 1 hr averaged U pα0/V A0 for each δ∣ B ∣rms/B 0 bin. The thick solid black curves show the theoretical effective thresholds U pα0,crit for the A/IC instability from Section 2. The vertical black line marks the amplitude above which our linear model breaks down, which is only the case in the first panel. The arrows in each panel below the abscissa indicate the amplitude δ∣ B ∣rms/B 0 = 0.2, the approximate limit of validity of the linear model.
Paper: Regulation of Proton–α Differential Flow by Compressive Fluctuations and Ion-scale Instabilities in the Solar Wind
Authors: Xingyu Zhu, Daniel Verscharen, Jiansen He, Bennett A. Maruca, Christopher J. Owen
Figure caption: Same as Figure 4 but using γ e = 1, γ p = 3, and γ  α  = 3. The vertical black lines mark in each panel the amplitude above which our linear model breaks down. The arrows in each panel below the abscissa indicate the amplitude δ∣ B ∣rms/B 0 = 0.2, the approximate limit of validity of the linear model.
Paper: Regulation of Proton–α Differential Flow by Compressive Fluctuations and Ion-scale Instabilities in the Solar Wind
Authors: Xingyu Zhu, Daniel Verscharen, Jiansen He, Bennett A. Maruca, Christopher J. Owen
Figure caption: Dependence of the maximum permitted U pα0 in terms of U pα0,crit/V A0 on β ∥p0 and δ B ∥/B 0 for the A/IC instability. The normalized amplitude δ B ∥/B 0 varies between 0 and 0.2.
Paper: Regulation of Proton–α Differential Flow by Compressive Fluctuations and Ion-scale Instabilities in the Solar Wind
Authors: Xingyu Zhu, Daniel Verscharen, Jiansen He, Bennett A. Maruca, Christopher J. Owen
Figure caption: Dependence of the maximum permitted U pα0 in terms of U pα0,crit/V A0 on β ∥p0 and δ B ∥/B 0 for the FM/W instability. The normalized amplitude δ B ∥/B 0 varies between 0 and 0.2.
Paper: Regulation of Proton–α Differential Flow by Compressive Fluctuations and Ion-scale Instabilities in the Solar Wind
Authors: Xingyu Zhu, Daniel Verscharen, Jiansen He, Bennett A. Maruca, Christopher J. Owen
Figure caption: Same as Figure 2 but using γ e = 1, γ p = 3, and γ  α  = 3.
Paper: Regulation of Proton–α Differential Flow by Compressive Fluctuations and Ion-scale Instabilities in the Solar Wind
Authors: Xingyu Zhu, Daniel Verscharen, Jiansen He, Bennett A. Maruca, Christopher J. Owen
Figure caption: Same as Figure 3 but using γ e = 1, γ p = 3, and γ  α  = 3.
Paper: Regulation of Proton–α Differential Flow by Compressive Fluctuations and Ion-scale Instabilities in the Solar Wind
Authors: Xingyu Zhu, Daniel Verscharen, Jiansen He, Bennett A. Maruca, Christopher J. Owen
Figure caption: Same as Figure 3 but using γ e = 1.18, γ p = 5/3, and γ  α  = 1.15.
Paper: Regulation of Proton–α Differential Flow by Compressive Fluctuations and Ion-scale Instabilities in the Solar Wind
Authors: Xingyu Zhu, Daniel Verscharen, Jiansen He, Bennett A. Maruca, Christopher J. Owen
Figure caption: Same as Figure 2 but using γ e = 1.18, γ p = 5/3, and γ  α  = 1.15.
Paper: Dynamics of Photospheric Magnetic Flux Distribution and Variations in Solar RVs: A Study Using HARPS-N Solar and SDO Observations
Authors: Anisha Sen, S. P. Rajaguru
Figure caption: Feature-specific disk-averaged unsigned field magnetic fluxes, (fB) m   =  f  m 〈∣B  m ∣〉, in the same order (top to bottom), with the overplotted black curves obtained in the same way, as in Figure 2. The insets are the same as explained in the caption of Figure 2.
Paper: Dynamics of Photospheric Magnetic Flux Distribution and Variations in Solar RVs: A Study Using HARPS-N Solar and SDO Observations
Authors: Anisha Sen, S. P. Rajaguru
Figure caption: Feature-specific fill factors, f  m , derived from full-disk SDO/HMI observations (top to bottom): weak IN (IN), strong network (NE), plage, and sunspot fields. The overplotted black curve in each panel is a smoothed one retaining only variations longer than 60 days obtained with a low-pass Fourier filter. The insets in each panel show a zoomed-in view of a selected 30-day window around a large increase in spot flux and its connections to other features.