adsabs/AstroCLIMB huggingface dataset:
Paper: A Dedicated System for Coordinated Radio and Optical Monitoring of the Space Weather of Young, Solar-type Stars
Authors: Ivey Davis, Gregg Hallinan, Navtej Saini, Casey Law, Yuping Huang, Rick Burruss, Jeffry Zolkower, John Baker, Curt Corcoran, Carolyn Heffner, Kathryn Plant, Nikita Kosogorov, Marin Anderson, Andrea Isella, Larry D'Addario, Jun Shi, Greg Hellbourg, David Hodge, Sandy Weinreb, Nivedita Mahesh, Ruby Byrne, Jack Hickish, Rick Hobbs, Mike Virgin, Ghislain Kemby, Corey Posner, John T. Klinefelter, Morgan Catha, James Lamb, Mark Hodges, Charlie Harnach, Vinand Prayag, David Woody, Andres Rizo, Andrew Romero-Wolf, Judd D. Bowman, Daniel C. Jacobs, Matthew Kolopanis, Katherine Elder, Akshatha K. Vydula, Dale Gary, Bin Chen, Surajit Mondal, Peijin Zhang, Sijie Yu, Sherry Chhabra, Brian O'Donnell, Jayce Dowell, Greg Taylor
Figure caption: Synthetic dynamic spectra for type III bursts with various values of a and α observed at the time and spectral resolution (256 ms, 24 kHz) of the OVRO-LWA SWAYS beam (top panels) and integrated up to the 10 s time resolution of slow-vis data (middle panels). The frequency-averaged light curves for the various beamformed (solid line) and slow-vis (dashed-line) dynamic spectra are shown in the bottom panel. These plots are meant to be representative of only the general shape of type III bursts and the effect of the integration time being larger than the duration of the event; the intensity of the burst at each pixel in the 256 ms resolution data was taken to be 1.5× the background intensity at every frequency channel and is not representative of the actual frequency dependence of burst intensity.
Paper: A Dedicated System for Coordinated Radio and Optical Monitoring of the Space Weather of Young, Solar-type Stars
Authors: Ivey Davis, Gregg Hallinan, Navtej Saini, Casey Law, Yuping Huang, Rick Burruss, Jeffry Zolkower, John Baker, Curt Corcoran, Carolyn Heffner, Kathryn Plant, Nikita Kosogorov, Marin Anderson, Andrea Isella, Larry D'Addario, Jun Shi, Greg Hellbourg, David Hodge, Sandy Weinreb, Nivedita Mahesh, Ruby Byrne, Jack Hickish, Rick Hobbs, Mike Virgin, Ghislain Kemby, Corey Posner, John T. Klinefelter, Morgan Catha, James Lamb, Mark Hodges, Charlie Harnach, Vinand Prayag, David Woody, Andres Rizo, Andrew Romero-Wolf, Judd D. Bowman, Daniel C. Jacobs, Matthew Kolopanis, Katherine Elder, Akshatha K. Vydula, Dale Gary, Bin Chen, Surajit Mondal, Peijin Zhang, Sijie Yu, Sherry Chhabra, Brian O'Donnell, Jayce Dowell, Greg Taylor
Figure caption: Log-scale, time-series-averaged images of the PSF (top) and the X- and Y-axis cross sections of the PSF for each individual image (bottom). The PSF with no diffuser (left), the 0﹩\mathop{.}\limits^{\unicode{x000b0}}﹩25 diffuser (center), and the 1° diffuser (right) are shown here. The full width at half-maxima (FWHMs) are indicated in the titles and reported in Table 4. White pixels are where either hot pixels, dead pixels, or high-rms pixels were flagged as determined from dark images. 50 frames were used for each of the averaged images.
Paper: A Dedicated System for Coordinated Radio and Optical Monitoring of the Space Weather of Young, Solar-type Stars
Authors: Ivey Davis, Gregg Hallinan, Navtej Saini, Casey Law, Yuping Huang, Rick Burruss, Jeffry Zolkower, John Baker, Curt Corcoran, Carolyn Heffner, Kathryn Plant, Nikita Kosogorov, Marin Anderson, Andrea Isella, Larry D'Addario, Jun Shi, Greg Hellbourg, David Hodge, Sandy Weinreb, Nivedita Mahesh, Ruby Byrne, Jack Hickish, Rick Hobbs, Mike Virgin, Ghislain Kemby, Corey Posner, John T. Klinefelter, Morgan Catha, James Lamb, Mark Hodges, Charlie Harnach, Vinand Prayag, David Woody, Andres Rizo, Andrew Romero-Wolf, Judd D. Bowman, Daniel C. Jacobs, Matthew Kolopanis, Katherine Elder, Akshatha K. Vydula, Dale Gary, Bin Chen, Surajit Mondal, Peijin Zhang, Sijie Yu, Sherry Chhabra, Brian O'Donnell, Jayce Dowell, Greg Taylor
Figure caption: A dynamic spectrum of the Sun, collected by the beamforming observing method of the OVRO-LWA (discussed in detail in Section 3.1.2). On the left, there is a collection of type III bursts and a type II burst. A close-up of a type III burst is shown on the right to show the sweeping structure evident at lower frequencies. Persistent, nondrifting emission above ≈50 MHz may be associated with type IV burst continuum emission.
Paper: A Dedicated System for Coordinated Radio and Optical Monitoring of the Space Weather of Young, Solar-type Stars
Authors: Ivey Davis, Gregg Hallinan, Navtej Saini, Casey Law, Yuping Huang, Rick Burruss, Jeffry Zolkower, John Baker, Curt Corcoran, Carolyn Heffner, Kathryn Plant, Nikita Kosogorov, Marin Anderson, Andrea Isella, Larry D'Addario, Jun Shi, Greg Hellbourg, David Hodge, Sandy Weinreb, Nivedita Mahesh, Ruby Byrne, Jack Hickish, Rick Hobbs, Mike Virgin, Ghislain Kemby, Corey Posner, John T. Klinefelter, Morgan Catha, James Lamb, Mark Hodges, Charlie Harnach, Vinand Prayag, David Woody, Andres Rizo, Andrew Romero-Wolf, Judd D. Bowman, Daniel C. Jacobs, Matthew Kolopanis, Katherine Elder, Akshatha K. Vydula, Dale Gary, Bin Chen, Surajit Mondal, Peijin Zhang, Sijie Yu, Sherry Chhabra, Brian O'Donnell, Jayce Dowell, Greg Taylor
Figure caption: A small fraction of the OVRO-LWA antennas for observing stellar plasma emission (left) and Flarescope for observing stellar flares (right). Here, EFA refers to the electronic focuser accessory, IRF90 is the rotational focuser, and OTA is the optical tube assembly; these elements as well as the rest of the Flarescope design are discussed in detail in Section 3.2.
Paper: A Dedicated System for Coordinated Radio and Optical Monitoring of the Space Weather of Young, Solar-type Stars
Authors: Ivey Davis, Gregg Hallinan, Navtej Saini, Casey Law, Yuping Huang, Rick Burruss, Jeffry Zolkower, John Baker, Curt Corcoran, Carolyn Heffner, Kathryn Plant, Nikita Kosogorov, Marin Anderson, Andrea Isella, Larry D'Addario, Jun Shi, Greg Hellbourg, David Hodge, Sandy Weinreb, Nivedita Mahesh, Ruby Byrne, Jack Hickish, Rick Hobbs, Mike Virgin, Ghislain Kemby, Corey Posner, John T. Klinefelter, Morgan Catha, James Lamb, Mark Hodges, Charlie Harnach, Vinand Prayag, David Woody, Andres Rizo, Andrew Romero-Wolf, Judd D. Bowman, Daniel C. Jacobs, Matthew Kolopanis, Katherine Elder, Akshatha K. Vydula, Dale Gary, Bin Chen, Surajit Mondal, Peijin Zhang, Sijie Yu, Sherry Chhabra, Brian O'Donnell, Jayce Dowell, Greg Taylor
Figure caption: Change in central source position on the detector (red and black dots) and the target elevation (blue line) over the course of a 6 hr observation. The tracking appears to become increasingly stable toward the peak of the target’s transit.
Paper: A Dedicated System for Coordinated Radio and Optical Monitoring of the Space Weather of Young, Solar-type Stars
Authors: Ivey Davis, Gregg Hallinan, Navtej Saini, Casey Law, Yuping Huang, Rick Burruss, Jeffry Zolkower, John Baker, Curt Corcoran, Carolyn Heffner, Kathryn Plant, Nikita Kosogorov, Marin Anderson, Andrea Isella, Larry D'Addario, Jun Shi, Greg Hellbourg, David Hodge, Sandy Weinreb, Nivedita Mahesh, Ruby Byrne, Jack Hickish, Rick Hobbs, Mike Virgin, Ghislain Kemby, Corey Posner, John T. Klinefelter, Morgan Catha, James Lamb, Mark Hodges, Charlie Harnach, Vinand Prayag, David Woody, Andres Rizo, Andrew Romero-Wolf, Judd D. Bowman, Daniel C. Jacobs, Matthew Kolopanis, Katherine Elder, Akshatha K. Vydula, Dale Gary, Bin Chen, Surajit Mondal, Peijin Zhang, Sijie Yu, Sherry Chhabra, Brian O'Donnell, Jayce Dowell, Greg Taylor
Figure caption: The Allan deviation, σA(τ) (defined in Equation (14)), derived from the airmass-corrected, normalized, 3 s cadence light curve for the full, 6 hr observation of pi UMa. Noise expectations for white noise and random-walk frequency modulation (RWFM) are indicated as dashed lines. Here, τ is the time that the original, 3 s cadence light curve is averaged over. The noises derived from the light curves produced from coadded images (shown in Figure 14) are plotted as open circles here. The noise from the 1 hr time frame that we consider in the rest of Section 4.3 is lower than the Allan variance from the full observation. This suggests that Flarescope (or at least its observing conditions) was particularly well behaved during the hour we evaluate in this section.
Paper: Extreme-ultraviolet Wave and Quasiperiodic Pulsations during an Eruptive M-class Flare
Authors: Shuyue Li, Qingmin Zhang, Haisheng Ji, Shengli Liu, Fanpeng Shi, Dong Li
Figure caption: (a1)–(c1) WL images of the CME observed by LASCO-C2 during 08:00−08:24 UT. (a2)–(c2) The same images as the top panels, with the projections of reconstructed cones being superposed with blue dots.
Paper: A Dedicated System for Coordinated Radio and Optical Monitoring of the Space Weather of Young, Solar-type Stars
Authors: Ivey Davis, Gregg Hallinan, Navtej Saini, Casey Law, Yuping Huang, Rick Burruss, Jeffry Zolkower, John Baker, Curt Corcoran, Carolyn Heffner, Kathryn Plant, Nikita Kosogorov, Marin Anderson, Andrea Isella, Larry D'Addario, Jun Shi, Greg Hellbourg, David Hodge, Sandy Weinreb, Nivedita Mahesh, Ruby Byrne, Jack Hickish, Rick Hobbs, Mike Virgin, Ghislain Kemby, Corey Posner, John T. Klinefelter, Morgan Catha, James Lamb, Mark Hodges, Charlie Harnach, Vinand Prayag, David Woody, Andres Rizo, Andrew Romero-Wolf, Judd D. Bowman, Daniel C. Jacobs, Matthew Kolopanis, Katherine Elder, Akshatha K. Vydula, Dale Gary, Bin Chen, Surajit Mondal, Peijin Zhang, Sijie Yu, Sherry Chhabra, Brian O'Donnell, Jayce Dowell, Greg Taylor
Figure caption: The entire, 6 hr optical light curve (starting at UTC 03:00:00 on 2024 April 10) at 5 minute integration time with 1σ ≈ 0.4 mmag error bars. The 3σ threshold is indicated by the dashed red line. A flare—modeled simply as a steep, linear rise and exponential decay with an e-folding time of 15 minutes—with a peak of 5σ was injected and is indicated by the solid line. The integration corresponding to the peak of this “flare” would correspond to an energy of ≈1033 erg, although the entire integrated profile (conservatively assuming a persistent flare temperature of 10,000 K) would correspond to an energy of 7.6 × 1033 erg.
Paper: Extreme-ultraviolet Wave and Quasiperiodic Pulsations during an Eruptive M-class Flare
Authors: Shuyue Li, Qingmin Zhang, Haisheng Ji, Shengli Liu, Fanpeng Shi, Dong Li
Figure caption: (a) SXR light curves of the flare in 1−8 (orange line) and 0.5−4 Å (blue line). (b) Time evolution of the heliocentric distances of the prominence leading front in the FOV of AIA (blue pluses), STB/EUVI (orange triangle), and in LASCO (red diamonds).
Paper: Extreme-ultraviolet Wave and Quasiperiodic Pulsations during an Eruptive M-class Flare
Authors: Shuyue Li, Qingmin Zhang, Haisheng Ji, Shengli Liu, Fanpeng Shi, Dong Li
Figure caption: The locations of STA (red circle), STB (green circle), and Earth (blue circle) on 2011 February 24. The separation angles of STA and STB with the Sun–Earth connection are 87﹩\mathop{.}\limits^{^\circ }﹩1 and 94﹩\mathop{.}\limits^{^\circ }﹩5, respectively.
Paper: A Dedicated System for Coordinated Radio and Optical Monitoring of the Space Weather of Young, Solar-type Stars
Authors: Ivey Davis, Gregg Hallinan, Navtej Saini, Casey Law, Yuping Huang, Rick Burruss, Jeffry Zolkower, John Baker, Curt Corcoran, Carolyn Heffner, Kathryn Plant, Nikita Kosogorov, Marin Anderson, Andrea Isella, Larry D'Addario, Jun Shi, Greg Hellbourg, David Hodge, Sandy Weinreb, Nivedita Mahesh, Ruby Byrne, Jack Hickish, Rick Hobbs, Mike Virgin, Ghislain Kemby, Corey Posner, John T. Klinefelter, Morgan Catha, James Lamb, Mark Hodges, Charlie Harnach, Vinand Prayag, David Woody, Andres Rizo, Andrew Romero-Wolf, Judd D. Bowman, Daniel C. Jacobs, Matthew Kolopanis, Katherine Elder, Akshatha K. Vydula, Dale Gary, Bin Chen, Surajit Mondal, Peijin Zhang, Sijie Yu, Sherry Chhabra, Brian O'Donnell, Jayce Dowell, Greg Taylor
Figure caption: The light curves from the background-subtracted data produced from the low-pass-filter method and the rolling-median method. Summing, rather than averaging, in frequency makes the severity of oversubtraction from the low-pass filtering more apparent. A ≈30 s inset in the bottom right corner is provided to demonstrate the failure of the low-pass method around strong, brief signals.
Paper: Extreme-ultraviolet Wave and Quasiperiodic Pulsations during an Eruptive M-class Flare
Authors: Shuyue Li, Qingmin Zhang, Haisheng Ji, Shengli Liu, Fanpeng Shi, Dong Li
Figure caption: Electron fluxes recoded by STB/IMPACT. The vertical orange line denotes 08:00 UT.
Paper: GRMHD Study of Accretion onto Time-like Naked Singularities
Authors: Akhil Uniyal, Indu K. Dihingia, Yosuke Mizuno, Włodek Kluźniak
Figure caption: Time evolution of integrated outflows (jet and wind) at r = 10 rg for different NkS objects. The jet and wind power are shown in (a), and their corresponding integrated electromagnetic and mass flux are shown in panels (b) and (c), respectively.
Paper: GRMHD Study of Accretion onto Time-like Naked Singularities
Authors: Akhil Uniyal, Indu K. Dihingia, Yosuke Mizuno, Włodek Kluźniak
Figure caption: Effective potential in the equatorial plane for specific angular momentum λ = 1.65. The NkS curves correspond to spacetime models as labeled in the legend (SS1.01 through JNW0.6 from left to right). The vertical dashed lines indicate the inner edge of the computational domain for the same models (Table 1).
Paper: GRMHD Study of Accretion onto Time-like Naked Singularities
Authors: Akhil Uniyal, Indu K. Dihingia, Yosuke Mizuno, Włodek Kluźniak
Figure caption: Effective potential in the poloidal plane for zero specific angular momentum, λ = 0. A Kerr BH and five different NkSs are shown.
Paper: GRMHD Study of Accretion onto Time-like Naked Singularities
Authors: Akhil Uniyal, Indu K. Dihingia, Yosuke Mizuno, Włodek Kluźniak
Figure caption: Azimuthal and time-averaged (t = 8000–10,000 tg) logarithmic density (ρ) for different NkS objects. The black and dashed white lines represent σ = 1 and −hut = 1.02, respectively.
Paper: GRMHD Study of Accretion onto Time-like Naked Singularities
Authors: Akhil Uniyal, Indu K. Dihingia, Yosuke Mizuno, Włodek Kluźniak
Figure caption: The volume-integrated mass accretion rate (﹩\dot{M}﹩), normalized magnetic flux (﹩\phi /\sqrt{| \dot{M}| }﹩), and magnetic flux (ϕ) for different NkSs at r = 10 rg are shown in panels (a1), (a2), and (a3), respectively. A black dashed horizontal line in panel (a2) corresponds to the MAD limit (﹩\phi /\sqrt{| \dot{M}| }﹩=15) (R. Narayan et al. 2003; J. C. McKinney et al. 2012; A. Tchekhovskoy & J. C. McKinney 2012).
Paper: GRMHD Study of Accretion onto Time-like Naked Singularities
Authors: Akhil Uniyal, Indu K. Dihingia, Yosuke Mizuno, Włodek Kluźniak
Figure caption: Ergosphere (the blue contour) and angular velocity color map in the poloidal plane for each NkS spacetime.
Paper: GRMHD Study of Accretion onto Time-like Naked Singularities
Authors: Akhil Uniyal, Indu K. Dihingia, Yosuke Mizuno, Włodek Kluźniak
Figure caption: Time-averaged (t = 8000–10,000 tg) logarithmic density (ρ) distribution at equatorial plane for different NkS objects. In each panel, the small-scale structure is shown by a close-up view around the singularity in the lower-right corner.
Paper: GRMHD Study of Accretion onto Time-like Naked Singularities
Authors: Akhil Uniyal, Indu K. Dihingia, Yosuke Mizuno, Włodek Kluźniak
Figure caption: Time-averaged (t = 8000–10,000 tg) logarithmic acceleration by gas pressure (agas), magnetic pressure (amag), and gravity (ag) for different NkS objects. In each panel, the small-scale structure is shown by a close-up view around the singularity in the lower-right corner.
Paper: X-Ray Emission Signatures of Galactic Feedback in the Hot Circumgalactic Medium: Predictions from Cosmological Hydrodynamical Simulations
Authors: Emily M. Silich, John ZuHone, Elena Bellomi, Cameron Hummels, Benjamin Oppenheimer, Philip F. Hopkins, Cassandra Lochhaas, Sam B. Ponnada, Alexey Vikhlinin
Figure caption: Edge-on projections of broadband thermal 0.5–1 keV X-ray surface brightness (XSB) for all galaxies in the sample sorted from lowest to highest halo mass (with ﹩\mathrm{log}(M\,[{M}_{\odot }])﹩ indicated in each bottom right corner). The XSB morphology in each galaxy is strongly dependent on the underlying galactic feedback physics and environment.
Paper: X-Ray Emission Signatures of Galactic Feedback in the Hot Circumgalactic Medium: Predictions from Cosmological Hydrodynamical Simulations
Authors: Emily M. Silich, John ZuHone, Elena Bellomi, Cameron Hummels, Benjamin Oppenheimer, Philip F. Hopkins, Cassandra Lochhaas, Sam B. Ponnada, Alexey Vikhlinin
Figure caption: Radial profiles calculated from broadband thermal 0.5–1 keV XSB edge-on projections of all galaxies in the sample. Profiles are calculated as the mean value in concentric circular annuli centered on the galaxy out to a radius of ≃200 kpc. For all galaxies except those incorporating cosmic-ray physics, the mean XSB profile slope is ∝r−3 (illustrated with multiple amplitudes for reference).
Paper: X-Ray Emission Signatures of Galactic Feedback in the Hot Circumgalactic Medium: Predictions from Cosmological Hydrodynamical Simulations
Authors: Emily M. Silich, John ZuHone, Elena Bellomi, Cameron Hummels, Benjamin Oppenheimer, Philip F. Hopkins, Cassandra Lochhaas, Sam B. Ponnada, Alexey Vikhlinin
Figure caption: Cylindrically averaged radial velocity profiles weighted by X-ray line emissivities (from top to bottom, O VII, O VIII, Fe XVII) for one galaxy from each simulation suite (from left to right, TNG, EAGLE, FIRE, FIRE2CR, FOGGIE, TEMPEST, SIMBA). Higher outflow velocity magnitudes are traced by higher-energy emission lines (e.g., Fe XVII). High-velocity biconical outflows are clearly illustrated for the galaxies from TNG50 and Simba (which incorporate AGN feedback), as well as from TEMPEST and FOGGIE (stellar feedback only). The EAGLE zoom and FIRE galaxies show evidence of smaller-scale outflows above and below the disk. A biconically oriented outflow is visible in the FIRE2CR galaxy at a somewhat low magnitude due to the relative lack of a resolved hot CGM phase in FIRE2CR runs.
Paper: X-Ray Emission Signatures of Galactic Feedback in the Hot Circumgalactic Medium: Predictions from Cosmological Hydrodynamical Simulations
Authors: Emily M. Silich, John ZuHone, Elena Bellomi, Cameron Hummels, Benjamin Oppenheimer, Philip F. Hopkins, Cassandra Lochhaas, Sam B. Ponnada, Alexey Vikhlinin
Figure caption: Top: mass probability distributions of hot gas for one galaxy from each simulation suite as a function of radial velocity and temperature. Bottom: O VIII luminosity distributions for the same. The histograms represent the corresponding distributions collapsed along the temperature axis. There exist high-temperature, high-velocity tails in the mass probability distributions for galaxies that exhibit strong feedback-driven biconical outflow features, which are traced strongly by the O VIII luminosity.
Paper: X-Ray Emission Signatures of Galactic Feedback in the Hot Circumgalactic Medium: Predictions from Cosmological Hydrodynamical Simulations
Authors: Emily M. Silich, John ZuHone, Elena Bellomi, Cameron Hummels, Benjamin Oppenheimer, Philip F. Hopkins, Cassandra Lochhaas, Sam B. Ponnada, Alexey Vikhlinin
Figure caption: Temperature vs. radial velocity phase diagrams for O VII, O VIII, and Fe XVII line luminosities in the TNG50-31 galaxy. The histograms represent the corresponding distributions collapsed along the temperature axis. For this galaxy—and in general—the luminosity of the highest-energy emission line (Fe XVII) peaks at higher temperatures than that of the lower-energy emission lines. For galaxies with hot, high-velocity outflows, this corresponds to also peaking at higher radial velocities.
Paper: X-Ray Emission Signatures of Galactic Feedback in the Hot Circumgalactic Medium: Predictions from Cosmological Hydrodynamical Simulations
Authors: Emily M. Silich, John ZuHone, Elena Bellomi, Cameron Hummels, Benjamin Oppenheimer, Philip F. Hopkins, Cassandra Lochhaas, Sam B. Ponnada, Alexey Vikhlinin
Figure caption: Comparisons of the “instantaneous” SFR per volume element as a function of galactic disk radius for galaxies simulated with only stellar (non-CR) feedback, sorted from lowest to highest mass (M200). Galaxies from the the FOGGIE and TEMPEST suites, which are simulated in Enzo with simple thermal stellar-feedback schemes, exhibit sharply peaked SFR in the central couple kiloparsecs of the disk center. The fiducial FIRE2 galaxies, which are simulated in Gizmo with a much more complex stellar-feedback model, have extended distributions of SFR out to ∼30 kpc.
Paper: X-Ray Emission Signatures of Galactic Feedback in the Hot Circumgalactic Medium: Predictions from Cosmological Hydrodynamical Simulations
Authors: Emily M. Silich, John ZuHone, Elena Bellomi, Cameron Hummels, Benjamin Oppenheimer, Philip F. Hopkins, Cassandra Lochhaas, Sam B. Ponnada, Alexey Vikhlinin
Figure caption: LOS velocity (vlos) weighted by the O VII (top panels) and Fe XVII (bottom panels) line emissivities for galaxies from each simulation suite (clockwise, from upper left for each, TNG (x2), FIRE, FIRE2CR, Simba, TEMPEST, FOGGIE, EAGLE) viewed from an intermediate projection. Here, velocity contributions from both rotation and outflows are visible, and the line weighting influences the observed velocity distribution.
Paper: X-Ray Emission Signatures of Galactic Feedback in the Hot Circumgalactic Medium: Predictions from Cosmological Hydrodynamical Simulations
Authors: Emily M. Silich, John ZuHone, Elena Bellomi, Cameron Hummels, Benjamin Oppenheimer, Philip F. Hopkins, Cassandra Lochhaas, Sam B. Ponnada, Alexey Vikhlinin
Figure caption: Example cylindrically averaged radial velocity profile weighted by the O VII X-ray line emissivity for TNG50-101. Centered on the galactic disk (green) in an edge-on orientation, positive velocities (pink) represent outward radial flows, and negative velocities (blue) represent inward radial flows.
Paper: X-Ray Emission Signatures of Galactic Feedback in the Hot Circumgalactic Medium: Predictions from Cosmological Hydrodynamical Simulations
Authors: Emily M. Silich, John ZuHone, Elena Bellomi, Cameron Hummels, Benjamin Oppenheimer, Philip F. Hopkins, Cassandra Lochhaas, Sam B. Ponnada, Alexey Vikhlinin
Figure caption: Radial profiles of vlos weighted by the O VII line emissivity derived from edge-on projections (e.g., within the 360 × 20 kpc extraction region shown for the FIRE2-m12i galaxy; top right) of all galaxies in the sample. This visualization maximizes contributions from rotational motions in the hot CGM.
Paper: X-Ray Emission Signatures of Galactic Feedback in the Hot Circumgalactic Medium: Predictions from Cosmological Hydrodynamical Simulations
Authors: Emily M. Silich, John ZuHone, Elena Bellomi, Cameron Hummels, Benjamin Oppenheimer, Philip F. Hopkins, Cassandra Lochhaas, Sam B. Ponnada, Alexey Vikhlinin
Figure caption: Comparison of the mass and O VIII luminosity profiles in temperature vs. vr space for emission models with CIE and CIE+photoionization in the FIRE2-m12i galaxy.
Paper: X-Ray Emission Signatures of Galactic Feedback in the Hot Circumgalactic Medium: Predictions from Cosmological Hydrodynamical Simulations
Authors: Emily M. Silich, John ZuHone, Elena Bellomi, Cameron Hummels, Benjamin Oppenheimer, Philip F. Hopkins, Cassandra Lochhaas, Sam B. Ponnada, Alexey Vikhlinin
Figure caption: Comparison of the mass and O VIII luminosity profiles in temperature vs. vr space for emission models with CIE and CIE+photoionization in the TNG50-211 galaxy.
Paper: What Determines the Brightness of the Magnetically Open Solar Corona?: Insights from Three-dimensional Radiative Magnetohydrodynamic Simulations and Observations
Authors: Haruhisa Iijima
Figure caption: Energy input (top) and dissipation rate (bottom) in the simulated solar corona. Shown are the dependence on the vertical magnetic flux imbalance (left) and the rms of the vertical magnetic field (right). The average is taken over the whole horizontal domain and the last 2 hr of each simulation.