adsabs/AstroCLIMB huggingface dataset:
Paper: Multimessenger Picture of J1048+7143 
Authors: Emma Kun, Ilja Jaroschewski, Armin Ghorbanietemad, Sándor Frey, Julia Becker Tjus, Silke Britzen, Krisztina Éva Gabányi, Vladimir Kiselev, Leander Schlegel, Marcel Schroller, Patrick Reichherzer, Lang Cui, Xin Wang, Yuling Shen
Figure caption: Left: the 4.8 GHz VLA image of J1048+7143 with the jet oriented to the west and extending to ∼15 kpc projected distance (red arrow). The peak brightness is 1.66 Jy beam−1, the lowest contours are at ±0.654 mJy beam−1 (∼3σ), and the positive contours increase by factors of 2. The elliptical Gaussian restoring beam is 0.″542 × 0.″392 with the position angle of the major axis PA = 6.2°. Middle and right: two examples of the 8.6 GHz jet structure observed with the VLBI. The angular scale of 1 mas corresponds to 8.361 pc projected linear scale. In the milliarcsecond-scale structure, there is an approximately eastern extension of the jet (turquoise arrow) and a southern one (green arrow), such that sometimes the eastern and sometimes the southern jet dominates, as discussed in the text. The image parameters in the middle are: observing date 2001 July 5, peak brightness 759 mJy beam−1, lowest contours ±0.76 mJy beam−1 (the positive contours increase by factors of 2), restoring beam 0.75 mas × 0.68 mas at PA = −20.3°. On the right: observing date 2010 March 23, peak brightness 882 mJy beam−1, lowest contours ±2.6 mJy beam−1 (the positive contours increase by factors of 2), restoring beam 0.81 mas × 0.66 mas at PA = 34.4°.
Paper: Multimessenger Picture of J1048+7143 
Authors: Emma Kun, Ilja Jaroschewski, Armin Ghorbanietemad, Sándor Frey, Julia Becker Tjus, Silke Britzen, Krisztina Éva Gabányi, Vladimir Kiselev, Leander Schlegel, Marcel Schroller, Patrick Reichherzer, Lang Cui, Xin Wang, Yuling Shen
Figure caption: Upper panel: the Fermi-LAT photon flux (186 MeV < E < 800 GeV) of 4FGL J1048.4+7143 as a function of time. Lower panel: the RATAN-600 4.8 GHz (purple filled circles), Nanshan 4.8 GHz (orange triangles), and OVRO 15 GHz single-dish radio flux density curves (blue empty diamonds), the 8.6 GHz integrated interferometric flux density of J1048+7143 (black empty diamonds), and the 8.6 GHz flux density of the VLBI core (black filled diamonds).
Paper: Multimessenger Picture of J1048+7143 
Authors: Emma Kun, Ilja Jaroschewski, Armin Ghorbanietemad, Sándor Frey, Julia Becker Tjus, Silke Britzen, Krisztina Éva Gabányi, Vladimir Kiselev, Leander Schlegel, Marcel Schroller, Patrick Reichherzer, Lang Cui, Xin Wang, Yuling Shen
Figure caption: Prediction of the fourth flare from J1048+7143 in the case of an SMBBH merger at its center. Red area: invalid flare prediction, as the merger would have already happened in the past. Gray area: duration of the first three flares detected with the errors in the duration. Blue area: predictions for the third and fourth flares. The prediction of the third flare (diagonal lines from lower left to upper right) is consistent with the time at which the actual flare was detected. The prediction of the fourth flare (diagonal lines from lower right to upper left) contains the purple area, which highlights a more probable time span based on the actual duration of the third detected flare.
Paper: Multimessenger Picture of J1048+7143 
Authors: Emma Kun, Ilja Jaroschewski, Armin Ghorbanietemad, Sándor Frey, Julia Becker Tjus, Silke Britzen, Krisztina Éva Gabányi, Vladimir Kiselev, Leander Schlegel, Marcel Schroller, Patrick Reichherzer, Lang Cui, Xin Wang, Yuling Shen
Figure caption: Gravitational wave signals from J1048+7143 on the condition of an SMBBH merger at its core. Blue and orange lines: expected characteristic strain with the mass ratios q = 1/5 and q = 1/30 respectively. Black lines: sensitivity curves from the detectors SKA, IPTA, and EPTA, constructed after Moore et al. (2015). Red line: LISA sensitivity curve, plotted following Robson et al. (2019). Vertical lines indicate the frequency of the gravitational wave emitted by a possible binary with (from left to right) 50 yr (yellow), 10 yr (magenta), 1 yr (cyan), and 30 days (purple) until the merger for the respective mass ratio.
Paper: Multimessenger Picture of J1048+7143 
Authors: Emma Kun, Ilja Jaroschewski, Armin Ghorbanietemad, Sándor Frey, Julia Becker Tjus, Silke Britzen, Krisztina Éva Gabányi, Vladimir Kiselev, Leander Schlegel, Marcel Schroller, Patrick Reichherzer, Lang Cui, Xin Wang, Yuling Shen
Figure caption: Date of the merger in the case of a supermassive binary black hole at the center of J1048+7143 as a function of the mass ratio of the binary q.
Paper: Multimessenger Picture of J1048+7143 
Authors: Emma Kun, Ilja Jaroschewski, Armin Ghorbanietemad, Sándor Frey, Julia Becker Tjus, Silke Britzen, Krisztina Éva Gabányi, Vladimir Kiselev, Leander Schlegel, Marcel Schroller, Patrick Reichherzer, Lang Cui, Xin Wang, Yuling Shen
Figure caption: Illustration of the centroid method applied to the γ-ray flux curve of J1048+7143. The sum of the contributions of the exponential flares fitted to the light curve is shown by a blue continuous line. Centers of the major flares (E > 168 MeV) are shown as green vertical dashed lines. The baseline is not shown because it has no impact on the duration or center of the flares.
Paper: Multimessenger Picture of J1048+7143 
Authors: Emma Kun, Ilja Jaroschewski, Armin Ghorbanietemad, Sándor Frey, Julia Becker Tjus, Silke Britzen, Krisztina Éva Gabányi, Vladimir Kiselev, Leander Schlegel, Marcel Schroller, Patrick Reichherzer, Lang Cui, Xin Wang, Yuling Shen
Figure caption: The spectral energy distribution (SED) of 4FGL J1048.4+7143 in the full Fermi-LAT time range.
Paper: Measurement of High-energy Cosmic-Ray Proton Spectrum from the ISS-CREAM Experiment
Authors: G. H. Choi, E. S. Seo, S. Aggarwal, Y. Amare, D. Angelaszek, D. P. Bowman, Y. C. Chen, M. Copley, L. Derome, L. Eraud, C. Falana, A. Gerrety, J. H. Han, H. G. Huh, A. Haque, Y. S. Hwang, H. J. Hyun, H. B. Jeon, J. A. Jeon, S. Jeong, S. C. Kang, H. J. Kim, K. C. Kim, M. H. Kim, H. Y. Lee, J. Lee, M. H. Lee, L. Lu, J. P. Lundquist, L. Lutz, A. Menchaca-Rocha, O. Ofoha, H. Park, I. H. Park, J. M. Park, N. Picot-Clemente, R. Scrandis, J. R. Smith, R. Takeishi, N. Vedenkin, P. Walpole, R. P. Weinmann, H. Wu, J. Wu, Z. Yin, Y. S. Yoon, H. G. Zhang
Figure caption: The measured charge distributions of proton and helium nuclei (a) for each layer (black solid line, top layer; green dashed line, second layer; blue dotted line, third layer) and (b) for the top layer with a double Landau-distribution fit (red dashed line). The red dotted lines represent distributions of each component of the proton and helium nuclei for this fit.
Paper: Measurement of High-energy Cosmic-Ray Proton Spectrum from the ISS-CREAM Experiment
Authors: G. H. Choi, E. S. Seo, S. Aggarwal, Y. Amare, D. Angelaszek, D. P. Bowman, Y. C. Chen, M. Copley, L. Derome, L. Eraud, C. Falana, A. Gerrety, J. H. Han, H. G. Huh, A. Haque, Y. S. Hwang, H. J. Hyun, H. B. Jeon, J. A. Jeon, S. Jeong, S. C. Kang, H. J. Kim, K. C. Kim, M. H. Kim, H. Y. Lee, J. Lee, M. H. Lee, L. Lu, J. P. Lundquist, L. Lutz, A. Menchaca-Rocha, O. Ofoha, H. Park, I. H. Park, J. M. Park, N. Picot-Clemente, R. Scrandis, J. R. Smith, R. Takeishi, N. Vedenkin, P. Walpole, R. P. Weinmann, H. Wu, J. Wu, Z. Yin, Y. S. Yoon, H. G. Zhang
Figure caption: An illustration of the shower axis reconstruction in CAL. The deposited energy in each ribbon is color coded. The largest signal in each layer is marked with an × symbol. The circled cross symbols are included in the final fit (red line).
Paper: Measurement of High-energy Cosmic-Ray Proton Spectrum from the ISS-CREAM Experiment
Authors: G. H. Choi, E. S. Seo, S. Aggarwal, Y. Amare, D. Angelaszek, D. P. Bowman, Y. C. Chen, M. Copley, L. Derome, L. Eraud, C. Falana, A. Gerrety, J. H. Han, H. G. Huh, A. Haque, Y. S. Hwang, H. J. Hyun, H. B. Jeon, J. A. Jeon, S. Jeong, S. C. Kang, H. J. Kim, K. C. Kim, M. H. Kim, H. Y. Lee, J. Lee, M. H. Lee, L. Lu, J. P. Lundquist, L. Lutz, A. Menchaca-Rocha, O. Ofoha, H. Park, I. H. Park, J. M. Park, N. Picot-Clemente, R. Scrandis, J. R. Smith, R. Takeishi, N. Vedenkin, P. Walpole, R. P. Weinmann, H. Wu, J. Wu, Z. Yin, Y. S. Yoon, H. G. Zhang
Figure caption: The overall efficiency ε as a function of the incident energy. The shaded area indicates associated uncertainties.
Paper: Measurement of High-energy Cosmic-Ray Proton Spectrum from the ISS-CREAM Experiment
Authors: G. H. Choi, E. S. Seo, S. Aggarwal, Y. Amare, D. Angelaszek, D. P. Bowman, Y. C. Chen, M. Copley, L. Derome, L. Eraud, C. Falana, A. Gerrety, J. H. Han, H. G. Huh, A. Haque, Y. S. Hwang, H. J. Hyun, H. B. Jeon, J. A. Jeon, S. Jeong, S. C. Kang, H. J. Kim, K. C. Kim, M. H. Kim, H. Y. Lee, J. Lee, M. H. Lee, L. Lu, J. P. Lundquist, L. Lutz, A. Menchaca-Rocha, O. Ofoha, H. Park, I. H. Park, J. M. Park, N. Picot-Clemente, R. Scrandis, J. R. Smith, R. Takeishi, N. Vedenkin, P. Walpole, R. P. Weinmann, H. Wu, J. Wu, Z. Yin, Y. S. Yoon, H. G. Zhang
Figure caption: The proton spectrum of the ISS-CREAM experiment (red filled circles) is compared with recent data from other experiments: AMS-02 (brown inverted triangles), combined CREAM-I and III (blue open circles), DAMPE (pink open diamonds), CALET (sky-blue open crosses), and NUCLEON (green open squares). For the ISS-CREAM proton spectrum, the error bars represent statistical uncertainties, and the shaded area is obtained by summing the statistical and systematic uncertainties in quadrature. The black line is the SBPL fit result from the energy range of 1.60 × 103–1.64 × 105 GeV.
Paper: Measurement of High-energy Cosmic-Ray Proton Spectrum from the ISS-CREAM Experiment
Authors: G. H. Choi, E. S. Seo, S. Aggarwal, Y. Amare, D. Angelaszek, D. P. Bowman, Y. C. Chen, M. Copley, L. Derome, L. Eraud, C. Falana, A. Gerrety, J. H. Han, H. G. Huh, A. Haque, Y. S. Hwang, H. J. Hyun, H. B. Jeon, J. A. Jeon, S. Jeong, S. C. Kang, H. J. Kim, K. C. Kim, M. H. Kim, H. Y. Lee, J. Lee, M. H. Lee, L. Lu, J. P. Lundquist, L. Lutz, A. Menchaca-Rocha, O. Ofoha, H. Park, I. H. Park, J. M. Park, N. Picot-Clemente, R. Scrandis, J. R. Smith, R. Takeishi, N. Vedenkin, P. Walpole, R. P. Weinmann, H. Wu, J. Wu, Z. Yin, Y. S. Yoon, H. G. Zhang
Figure caption: The ISS-CREAM proton spectrum is compared with calculations by Zatsepin & Sokolskaya (2006), blue dashed line; Gaisser et al. (2013), black solid line; Ptuskin et al. (2013), green dotted line.
Paper: Measurement of High-energy Cosmic-Ray Proton Spectrum from the ISS-CREAM Experiment
Authors: G. H. Choi, E. S. Seo, S. Aggarwal, Y. Amare, D. Angelaszek, D. P. Bowman, Y. C. Chen, M. Copley, L. Derome, L. Eraud, C. Falana, A. Gerrety, J. H. Han, H. G. Huh, A. Haque, Y. S. Hwang, H. J. Hyun, H. B. Jeon, J. A. Jeon, S. Jeong, S. C. Kang, H. J. Kim, K. C. Kim, M. H. Kim, H. Y. Lee, J. Lee, M. H. Lee, L. Lu, J. P. Lundquist, L. Lutz, A. Menchaca-Rocha, O. Ofoha, H. Park, I. H. Park, J. M. Park, N. Picot-Clemente, R. Scrandis, J. R. Smith, R. Takeishi, N. Vedenkin, P. Walpole, R. P. Weinmann, H. Wu, J. Wu, Z. Yin, Y. S. Yoon, H. G. Zhang
Figure caption: The deconvolution matrix for protons.
Paper: Measurement of High-energy Cosmic-Ray Proton Spectrum from the ISS-CREAM Experiment
Authors: G. H. Choi, E. S. Seo, S. Aggarwal, Y. Amare, D. Angelaszek, D. P. Bowman, Y. C. Chen, M. Copley, L. Derome, L. Eraud, C. Falana, A. Gerrety, J. H. Han, H. G. Huh, A. Haque, Y. S. Hwang, H. J. Hyun, H. B. Jeon, J. A. Jeon, S. Jeong, S. C. Kang, H. J. Kim, K. C. Kim, M. H. Kim, H. Y. Lee, J. Lee, M. H. Lee, L. Lu, J. P. Lundquist, L. Lutz, A. Menchaca-Rocha, O. Ofoha, H. Park, I. H. Park, J. M. Park, N. Picot-Clemente, R. Scrandis, J. R. Smith, R. Takeishi, N. Vedenkin, P. Walpole, R. P. Weinmann, H. Wu, J. Wu, Z. Yin, Y. S. Yoon, H. G. Zhang
Figure caption: Exploded view of the ISS-CREAM instrument (Seo et al. 2014).
Paper: Cosmological Simulation of Galaxy Groups and Clusters. II. Studying Different Modes of Feedback through X-Ray Observations
Authors: Rudrani Kar Chowdhury, Suchetana Chatterjee, Ankit Paul, Craig L. Sarazin, Jane Lixin Dai
Figure caption: Stacked X-ray surface brightness profiles of diffuse gas surrounding the AGN population having different feedback modes. Left: radial profile of stacked X-ray emission from the diffuse gas around the AGN with different modes of feedback at z = 1 modeled theoretically using APEC. Right: same as the left panel except at very low redshift (z = 0.016). Color schemes are the same in both panels. Green crosses represent the scenario when no AGN feedback is present in the systems. Black diamonds stand for AGNs having only the radiative wind mode of feedback. Blue stars are representative of the cases when both jet and radiative wind modes of feedback are active in the AGN. Red dots show the scenario when all radiative wind, jet, and X-ray feedback are present in the simulation. The figure shows that both jet and X-ray feedback are effective at dispersing the surrounding hot gas, but that the radiative wind mode alone is not (see Section 3).
Paper: Cosmological Simulation of Galaxy Groups and Clusters. II. Studying Different Modes of Feedback through X-Ray Observations
Authors: Rudrani Kar Chowdhury, Suchetana Chatterjee, Ankit Paul, Craig L. Sarazin, Jane Lixin Dai
Figure caption: X-ray maps of hot gas in the simulations of different feedback modes in regions of radii 50 h −1 kpc having the AGN at the center at z = 1. Color bars show the emitted X-ray surface brightness in erg cm−2 s−1 calculated using APEC in the soft band (0.5–2 keV). This is discussed in Section 2.1. Top left: theoretical X-ray map in the presence of all AGN feedback modes. Top right: X-ray map of the hot gas in the vicinity of an AGN in which both the jet and radiative wind modes of feedback are operative but the X-ray feedback mode is absent. Bottom left: diffuse X-ray map around the same AGN having only the radiative wind feedback mode. Bottom right: theoretical X-ray map of diffuse gas surrounding the same system having no AGN feedback. The statistical results are discussed in Section 3.
Paper: Cosmological Simulation of Galaxy Groups and Clusters. II. Studying Different Modes of Feedback through X-Ray Observations
Authors: Rudrani Kar Chowdhury, Suchetana Chatterjee, Ankit Paul, Craig L. Sarazin, Jane Lixin Dai
Figure caption: Stacked synthetic X-ray surface brightness profiles for different AGN feedback scenarios. Left: stacked radial profile of X-ray surface brightness obtained from mock observation of diffuse gas surrounding AGNs having different modes of feedback at z = 1. Right: same as the left panel but at very low redshift (z = 0.016). The color scheme is the same in both panels. Green diamonds represent the scenario when no AGN feedback is present in the systems. Red lines show the systems having only the radiative wind mode of feedback. Black dots stand for AGNs in which both the radiative wind and jet modes of feedback are active but X-ray feedback is absent. Finally, blue stars are representative of AGNs having all three modes of feedback. We notice that different modes of AGN feedback are difficult to disentangle in the very central region of the high-redshift objects. However, in the low-redshift objects, we see a significant decrement of the X-ray surface brightness in the central region when all the feedback modes are included. See Section 3.3 for details.
Paper: Cosmological Simulation of Galaxy Groups and Clusters. II. Studying Different Modes of Feedback through X-Ray Observations
Authors: Rudrani Kar Chowdhury, Suchetana Chatterjee, Ankit Paul, Craig L. Sarazin, Jane Lixin Dai
Figure caption: X-ray maps of hot gas in the simulations of different feedback modes in regions of radii 50 h −1 kpc having the AGN at the center at z = 0.016. Here also color bars represent theoretical X-ray surface brightness in the soft energy band (0.5–2 keV) in units of erg cm−2 s−1 in all the panels. All four panels have the same layout as in Figure 1. The linear feature visible in the top right panel, where jet and radiative wind modes of feedback are present, could be the signature of a double-sided jet emitted by the AGN at the center. The stacking analysis is described in Section 3.
Paper: Cosmological Simulation of Galaxy Groups and Clusters. II. Studying Different Modes of Feedback through X-Ray Observations
Authors: Rudrani Kar Chowdhury, Suchetana Chatterjee, Ankit Paul, Craig L. Sarazin, Jane Lixin Dai
Figure caption: Zoomed-in image of synthetic Chandra X-ray maps of the systems shown in Figure 1 within the region of radius 50 h −1 kpc ( ∼ 6.″5) at z = 1. In all panels color bars represent the photon number counts per pixel, where the pixel size is ∼0.″5. Top left: mock X-ray map of the diffuse gas around an AGN having all the feedback modes. Top right: synthetic X-ray map of hot gas in the vicinity of an AGN that provides radiative wind as well as jet feedback to its ambient medium. Bottom left: diffuse X-ray map of a synthetic observation surrounding an AGN in which only the radiative wind mode of feedback is present but jet and X-ray feedback are absent. Bottom right: mock X-ray map surrounding a black hole having no feedback mode. See Section 3.3 for discussions.
Paper: Cosmological Simulation of Galaxy Groups and Clusters. II. Studying Different Modes of Feedback through X-Ray Observations
Authors: Rudrani Kar Chowdhury, Suchetana Chatterjee, Ankit Paul, Craig L. Sarazin, Jane Lixin Dai
Figure caption: Stacked radial profiles of various gas properties. Top row: density profiles of gas surrounding the black holes offering different modes of feedback to their ambient medium. Second row: stacked radial profiles of temperature in the presence of various feedback modes. Third row: entropy profiles in different AGN feedback mode scenarios. Bottom row: radial pressure profiles in the presence of different AGN feedback modes. Left and right panels represent the profiles at z = 1 and z = 0.016 respectively. The color scheme is the same in all panels, and different colors show different feedback modes similar to Figure 4.
Paper: Cosmological Simulation of Galaxy Groups and Clusters. II. Studying Different Modes of Feedback through X-Ray Observations
Authors: Rudrani Kar Chowdhury, Suchetana Chatterjee, Ankit Paul, Craig L. Sarazin, Jane Lixin Dai
Figure caption: Zoomed-in image of synthetic Chandra maps corresponding to the low-redshift systems (z = 0.016) shown in Figure 2 within a region of 50 h −1 kpc radius ﹩(\sim 2\buildrel{\,\prime}\over{.} 5)﹩. Color bars represent the photon number counts per pixel. The different panels have the same feedback parameters as Figure 6.
Paper: Cosmological Simulation of Galaxy Groups and Clusters. II. Studying Different Modes of Feedback through X-Ray Observations
Authors: Rudrani Kar Chowdhury, Suchetana Chatterjee, Ankit Paul, Craig L. Sarazin, Jane Lixin Dai
Figure caption: Distribution of characteristic mass (top) and radius (bottom) of the host dark matter halos of AGNs used for stacking in Figure 4. Left and right panels show the distribution at z = 1 and z = 0.016 respectively. In all the panels black, magenta, cyan, and red respectively represent the scenario where all, radiative wind and jet, only radiative wind, and no AGN feedback modes are present.
Paper: Cosmological Simulation of Galaxy Groups and Clusters. II. Studying Different Modes of Feedback through X-Ray Observations
Authors: Rudrani Kar Chowdhury, Suchetana Chatterjee, Ankit Paul, Craig L. Sarazin, Jane Lixin Dai
Figure caption: Contribution of the central AGN to the diffuse X-ray emission. Left and right panels show the example of one system at z = 1 and z = 0.016 respectively. The color scheme is the same in both panels. Red stars represent the extended X-ray emission from the gas surrounding the AGN whereas black diamonds represent the X-ray emission coming from the central AGN itself. It can be seen that at the very central pixel the AGN contribution is dominating the diffuse X-ray emission. See discussions in Section 3.3.
Paper: Orbital Decay of Double White Dwarfs: Beyond Gravitational-wave Radiation Effects
Authors: G. A. Carvalho, R. C. dos Anjos, J. G. Coelho, R. V. Lobato, M. Malheiro, R. M. Marinho, J. F. Rodriguez, J. A. Rueda, R. Ruffini
Figure caption: Constraints on the binary masses and magnetic field for SDSS J0651+2844. We have used the values inferred from photometric and spectroscopic measurements of the orbital period, decay rate, and masses reported in Hermes et al. (2012) (see also Table 1). The blue rectangle represents the 1σ uncertainties on the masses. Left: constraints considering the lower limit for the decay rate, ﹩\dot{P}=-(9.8-2.8)\times {10}^{-12}﹩ s s−1, which gives the lower limit to the contribution of ﹩\tilde{B}﹩ and tides. Pure GW radiation is consistent with 1σ errors in the masses. Center: constraints considering the central value of the decay rate, ﹩\dot{P}=-9.8\times {10}^{-12}﹩ s s−1. Right: constraints considering the upper limit for the decay rate, ﹩\dot{P}=-(9.8+2.8)\times {10}^{-12}﹩ s s−1, which we use to estimate the upper limit on ﹩\tilde{B}﹩. Summarizing, the current decay rate is consistent with a pure GW-driven dynamics, but the uncertainties on the mass measurements and ﹩\dot{P}﹩ are broad enough to allow solutions of GW emission admixed with a UI and tides, although the absence of Zeeman splitting in the spectra rule out magnetic field strengths B > 106 G.
Paper: Orbital Decay of Double White Dwarfs: Beyond Gravitational-wave Radiation Effects
Authors: G. A. Carvalho, R. C. dos Anjos, J. G. Coelho, R. V. Lobato, M. Malheiro, R. M. Marinho, J. F. Rodriguez, J. A. Rueda, R. Ruffini
Figure caption: Examples of numerical solution of the equations of motion, Equations (2)–(3), for selected values of the primary’s magnetic field. In these examples, we set η = 100, the binary is mass-symmetric with M 1 = M 2 = 0.6 M ⊙, and we assign an initial (t = 0) values for the orbital period and the degree of synchronization of the primary, respectively, ﹩P(0)=10\,\min ﹩ (i.e., ω 0(0) = 0.0105) and α(0) = 0.5. The mass–radius relation is taken from Carvalho et al. (2018). For comparison, we also show the solution of the equations of motion when only GW radiation is considered, i.e., the solution to Equation (17). Upper left: orbital evolution, ω 0. Upper right: orbital decay rate, ﹩\dot{P}﹩, normalized to the value for the case of only GW radiation, ﹩{\dot{P}}_{\mathrm{GW}}﹩. Lower left: evolution of the primary’s synchronization, α. Lower right: evolution of the twist parameter, ξ  ϕ .
Paper: Inconspicuous Solar Polar Coronal X-Ray Jets as the Source of Conspicuous Hinode/EUV Imaging Spectrometer Doppler Outflows
Authors: Alphonse C. Sterling, Conrad Schwanitz, Louise K. Harra, Nour E. Raouafi, Navdeep K. Panesar, Ronald L. Moore
Figure caption: EIS-observed Doppler outflow events for the five events studied here, in the Fe XII 195.12 Å emission line. These are the first five events studied in Schwanitz et al. (2021), with the event number (which also corresponds to the event numbers of this paper) given in the upper right of each panel, and with each event’s date and time of the center of the Doppler outflow observations given at the top of each panel in DD-MM-YYYY HH:MM format. Deep blue features inside the contours represent observed outflows in excess of Doppler velocity −6 km s−1. See Section 2 and Schwanitz et al. (2021) for other details.