adsabs/AstroCLIMB huggingface dataset:
Paper: Periodic Oscillations in LASCO Coronal Mass Ejection Speeds: Space Seismology
Authors: Grzegorz Michalek, Nat Gopalswamy, and Seiji Yashiro
Figure caption: Temporal evolution of average annual values of solar spot numbers (panel a), speed of CMEs revealing oscillations (panel b), periods of oscillations (panel c), and their amplitudes (panel d). Error bars show the standard deviation for a given sample. Dashed lines in panels (c) and (d) represent the results obtained with a reduced cadence of height–time points to match the SC 23 cadence.
Paper: Core Electron Heating by Triggered Ion Acoustic Waves in the Solar Wind
Authors: F. S. Mozer, S. D. Bale, C. A. Cattell, J. Halekas, I. Y. Vasko, J. L. Verniero, and P. J. Kellogg
Figure caption: Plasma parameters during perihelion passes 6 and 8 of the Parker Solar Probe. Note that after the first day of orbit 6, the electron temperature followed the red curve of minimum temperature even though the solar wind speed varied from 300 to 800 km s−1.
Paper: Core Electron Heating by Triggered Ion Acoustic Waves in the Solar Wind
Authors: F. S. Mozer, S. D. Bale, C. A. Cattell, J. Halekas, I. Y. Vasko, J. L. Verniero, and P. J. Kellogg
Figure caption: Triggered and normal ion acoustic waves observed during orbit 6. The triggered ion acoustic waves (panel 2A) were associated with large TE/TI (panel 2B) and heated electrons (panel 2C). Note that the triggered ion acoustic waves were narrowband in frequency and of long duration (hours) while the normal ion acoustic waves during the one minute interval of panel 2D were broadband waves of short duration.
Paper: Core Electron Heating by Triggered Ion Acoustic Waves in the Solar Wind
Authors: F. S. Mozer, S. D. Bale, C. A. Cattell, J. Halekas, I. Y. Vasko, J. L. Verniero, and P. J. Kellogg
Figure caption: Plasma parameters during perihelion passes 7 and 9 of the Parker Solar Probe. Note that the electron temperature was approximately equal to but not less than the red curve of minimum temperature in the absence of waves, and that it exceeded the red curve by as much as a factor of two near triggered ion acoustic waves.
Paper: Core Electron Heating by Triggered Ion Acoustic Waves in the Solar Wind
Authors: F. S. Mozer, S. D. Bale, C. A. Cattell, J. Halekas, I. Y. Vasko, J. L. Verniero, and P. J. Kellogg
Figure caption: The inbound (panels 4A–4D) and outbound (panels 4E–4H) passes of orbit 7, illustrating the electric field, temperature ratio, electron temperature, and the plasma velocity. The red curves of minimum temperature in panels 4C and 4G give the decreases in electron temperature with distance expected for adiabatic expansion of the electron gas without heating. Their differences from the measured temperatures (the black curves) show that electrons were heated in regions containing triggered ion acoustic waves (panels 4A and 4E) and large ratios of electron to ion temperature (panels 4B and 4F).
Paper: Core Electron Heating by Triggered Ion Acoustic Waves in the Solar Wind
Authors: F. S. Mozer, S. D. Bale, C. A. Cattell, J. Halekas, I. Y. Vasko, J. L. Verniero, and P. J. Kellogg
Figure caption: The core electron and ion temperatures vs. solar radius, as determined from the eight passes of the Parker Solar Probe through the region of 15–40 solar radii on orbits 6–9. Each curve gives the one-hour running average of some 10,000,000 raw data points. The red curves of minimum temperature give the radial variation of the temperature for adiabatic expansion with no heating. The deviation between the core electron temperatures and the red curve in the left panel shows that electrons were heated in the region of 20–25 solar radii. Because the ion temperature depended much more strongly on the solar wind speed than did the electron temperature, it is not possible to determine the ion heating in the right panel without correcting for the dependence of the ion temperature on the solar wind speed.
Paper: Core Electron Heating by Triggered Ion Acoustic Waves in the Solar Wind
Authors: F. S. Mozer, S. D. Bale, C. A. Cattell, J. Halekas, I. Y. Vasko, J. L. Verniero, and P. J. Kellogg
Figure caption: Features of triggered ion acoustic waves, including the electric field having higher frequency pulses in phase with a wave of a few hertz (panel 6A), low- and high-frequency density fluctuations in sync with the electric fields (panels 6B and 6C), the absence of magnetic field signatures of a similar frequency (panel 6D), and with the higher frequency electric field and density fluctuations being narrowband signals (panels 6E and 6F).
Paper: The Rotation of Magnetic Flux Ropes Formed during Solar Eruption
Authors: Zhenjun Zhou, Chaowei Jiang, Rui Liu, Yuming Wang, Lijuan Liu, and Jun Cui
Figure caption: Panel (a) shows a reverse-S-shaped filament observed by GONG/Hα on 2012 May 10 at 00:00 UT. The corresponding sigmoid observed by Hinode/XRT is shown in (b). In panel (c), the green plus symbols outlining the EUV filament spine are projected onto an HMI magnetogram of the local Br.
Paper: The Rotation of Magnetic Flux Ropes Formed during Solar Eruption
Authors: Zhenjun Zhou, Chaowei Jiang, Rui Liu, Yuming Wang, Lijuan Liu, and Jun Cui
Figure caption: (a) Streamlines of the magnetic field at the central plane at t = 28 minutes, showing the cross section of the MFR. Panels (b)–(d) Evolutions of the MFR’s axis (red) and one twisted field line (green) wrapping around the axis.
Paper: The Rotation of Magnetic Flux Ropes Formed during Solar Eruption
Authors: Zhenjun Zhou, Chaowei Jiang, Rui Liu, Yuming Wang, Lijuan Liu, and Jun Cui
Figure caption: Evolution of the parameters in the simulation. Top panel (a): temporal evolution of twist (black line) and nonlocal writhe (red line) of the flux rope during its eruption. In the inset panel, the green line shows the temporal changing rate of the linking number (﹩{{ \mathcal L }}_{k}﹩). Bottom panel (b): the temporal change ratios of the free magnetic energy E (black line) and relative magnetic helicity H (blue line) compared with that of the eruption onset. For reference, at the onset of the eruption, the magnetic free energy is 0.91 of the corresponding potential magnetic energy, and the relative helicity is −0.06 as normalized by the square of the total unsigned magnetic flux.
Paper: NGC 5846-UDG1: A Galaxy Formed Mostly by Star Formation in Massive, Extremely Dense Clumps of Gas
Authors: Shany Danieli, Pieter van Dokkum, Sebastian Trujillo-Gomez, J. M. Diederik Kruijssen, Aaron J. Romanowsky, Scott Carlsten, Zili Shen, Jiaxuan Li, Roberto Abraham, Jean Brodie, Charlie Conroy, Jonah S. Gannon, Johnny Greco
Figure caption: The ICMF models constrain the origin of NGC 5846-UDG1's globular cluster system. Left panel: constraints on the ICMF of NGC 5846-UDG1, based on its present-day observed globular clusters and total stellar mass. The observed GCMF, corrected for mass loss due to stellar evolution, is shown by the black histogram. The fiducial model, constrained by the environmental dependence of the fraction of star formation in bound clusters (i.e., the CFE; Kruijssen 2012), is shown as the shaded purple band for a range of Toomre Q disk stability parameters (0.5 ≤ Q ≤ 3.0), where the purple dotted–dashed curve corresponds to Q = 0.5. For reference, the black solid and dashed gray curves show the minimum and maximum CFE models, respectively. The minimum CFE model assumes that the present-day globular clusters were the only clusters that formed, whereas the maximum CFE model assumes that all stars in the galaxy came from disrupted low-mass clusters. The mass functions are weighted by mass, so that the area under each curve is directly proportional to the mass in clusters. Right panel: cumulative fraction of galaxy mass in clusters at the time of formation for NGC 5846-UDG1 in comparison to the Milky Way. For NGC 5846-UDG1, the purple dotted–dashed curve shows the fiducial model (constrained by the CFE), and the black solid curve shows the present-day observed fraction. The orange dashed curve assumes no mass loss or cluster disruption for the Milky Way globular clusters, correcting only for mass loss due to stellar evolution. The fraction of galaxy mass in clusters in NGC 5846-UDG1 is 2–3 orders of magnitude higher than in the Milky Way, irrespective of the adopted CFE model.
Paper: NGC 5846-UDG1: A Galaxy Formed Mostly by Star Formation in Massive, Extremely Dense Clumps of Gas
Authors: Shany Danieli, Pieter van Dokkum, Sebastian Trujillo-Gomez, J. M. Diederik Kruijssen, Aaron J. Romanowsky, Scott Carlsten, Zili Shen, Jiaxuan Li, Roberto Abraham, Jean Brodie, Charlie Conroy, Jonah S. Gannon, Johnny Greco
Figure caption: Left panel: background-subtracted globular cluster luminosity function of NGC 5846-UDG1 in absolute magnitude (gray histogram) and its best-fit Gaussian luminosity function (red curve). Right panel: absolute magnitude in globular clusters vs. total magnitude of the host galaxy. Diagonal lines show constant globular cluster–to–field star light fractions ranging from 0.1% to 13%. Shown by a red star, NGC 5846-UDG1 has the highest fraction of stars in globular clusters known to date (12.9% ± 0.6%). This is measured with high certainty, demonstrated with the small error bar (0.05 mag) on top of the star. Some Coma UDGs (open circles) are excellent candidates for sharing a similar high fraction of stars in globular clusters, but these are four times farther away and thus 16 times fainter and have commensurately larger error bars.
Paper: Early Warnings of Binary Neutron Star Coalescence Using the SPIIR Search
Authors: Manoj Kovalam, Md Anwarul Kaium Patwary, Anala K. Sreekumar, Linqing Wen, Fiona H. Panther, Qi Chu
Figure caption: Accuracy of chirp mass and S/N recovery for the 0 s, −30 s, and −60 s configurations. Top panel: distributions for fractional differences in the recovered and injected chirp masses. The error margin is within 2% for all the runs. Bottom panel: distributions for fractional differences in recovered and expected S/Ns. About half of all events fall within the 10% error margin (in the bottom panel), of which 3% can be attributed to the SPIIR GW waveform approximation.
Paper: Early Warnings of Binary Neutron Star Coalescence Using the SPIIR Search
Authors: Manoj Kovalam, Md Anwarul Kaium Patwary, Anala K. Sreekumar, Linqing Wen, Fiona H. Panther, Qi Chu
Figure caption: Box and whiskers plot comparing the searched and 90% credible areas for all the runs. The y-axis represents the localization areas, and the x-axis represents the truncation latency for each EW run. The boxes encompass 95% of the events and the whiskers extend up to the rest. The white lines within the boxes represent the median values of the respective data sets. Using simulated Gaussian data, we demonstrate that the median searched areas are several times lower than the 90% credible areas, implying that a lot less area (as compared to the 90% credible region) can be searched to localize the GW event in O4.
Paper: Early Warnings of Binary Neutron Star Coalescence Using the SPIIR Search
Authors: Manoj Kovalam, Md Anwarul Kaium Patwary, Anala K. Sreekumar, Linqing Wen, Fiona H. Panther, Qi Chu
Figure caption: Searched areas vs. the number of detected events in each EW configuration as the cumulative fraction of the total number of full-bandwidth detection (left y-axis). The secondary y-axis shows the same as a function of the expected number of BNS detections per year in O4. Each color represents one EW configuration. Using a simulated Gaussian environment for O4, we expect to recover at least 1 (6%) premerger event per year with a localization area of <300 deg2 with the H1L1 configuration in O4.
Paper: Early Warnings of Binary Neutron Star Coalescence Using the SPIIR Search
Authors: Manoj Kovalam, Md Anwarul Kaium Patwary, Anala K. Sreekumar, Linqing Wen, Fiona H. Panther, Qi Chu
Figure caption: Evolution of S/Ns at different premerger latencies in simulated LIGO O4 data for a 1.4 M ⊙–1.4 M ⊙ BNS system at a distance of 100 Mpc. The dotted line represents the theoretical S/Ns calculated using matched filtering while the symbols show S/Ns from the SPIIR method. A strong event with a full-bandwidth S/N of 30 can be detected at subminute premerger latencies.
Paper: NGC 5846-UDG1: A Galaxy Formed Mostly by Star Formation in Massive, Extremely Dense Clumps of Gas
Authors: Shany Danieli, Pieter van Dokkum, Sebastian Trujillo-Gomez, J. M. Diederik Kruijssen, Aaron J. Romanowsky, Scott Carlsten, Zili Shen, Jiaxuan Li, Roberto Abraham, Jean Brodie, Charlie Conroy, Jonah S. Gannon, Johnny Greco
Figure caption: Photometric selection criteria for globular clusters in NGC 5846-UDG1. Left panel: all sources within 2 × r eff in the color–magnitude plane. All sources have sizes proportional to their FWHM sizes measured in pixels. Sources that met the selection criteria are shown by filled circles, and open circles are sources that were not selected. The three dashed boxes show the different color criteria as a function of the F606W magnitude. Right panel: same as the left panel for a background field with a similar area. There is only one contaminating source (filled circle) with m F606W < 25.0 mag. For fainter sources (m F606W > 25.0 mag), the number of contaminating objects increases, and these are accounted for in the calculation of the total globular cluster number.
Paper: NGC 5846-UDG1: A Galaxy Formed Mostly by Star Formation in Massive, Extremely Dense Clumps of Gas
Authors: Shany Danieli, Pieter van Dokkum, Sebastian Trujillo-Gomez, J. M. Diederik Kruijssen, Aaron J. Romanowsky, Scott Carlsten, Zili Shen, Jiaxuan Li, Roberto Abraham, Jean Brodie, Charlie Conroy, Jonah S. Gannon, Johnny Greco
Figure caption: First panel (from left to right): 47″ × 47″ DECaLS r-band cutout centered on NGC 5846-UDG1. Second panel: same cutout after MRF. High surface brightness and compact sources were subtracted and masked. Third panel: two-dimensional Sérsic best-fit model obtained using the pymfit code. The best-fit model parameters are shown in the blue text. Fourth panel: residual image after subtracting the galaxy model.
Paper: NGC 5846-UDG1: A Galaxy Formed Mostly by Star Formation in Massive, Extremely Dense Clumps of Gas
Authors: Shany Danieli, Pieter van Dokkum, Sebastian Trujillo-Gomez, J. M. Diederik Kruijssen, Aaron J. Romanowsky, Scott Carlsten, Zili Shen, Jiaxuan Li, Roberto Abraham, Jean Brodie, Charlie Conroy, Jonah S. Gannon, Johnny Greco
Figure caption: Upper image: V-band image taken with the WFC3 UVIS channel. All sources are masked except for the smooth diffuse light component of NGC 5846-UDG1 and its globular cluster candidates. About 13% of all stars reside in NGC 5846-UDG1's globular clusters, and both components have similar spatial distributions. Lower right image: F606W−F475W combined color image. Globular clusters brighter than M F606W = −7.6 mag have a median g − V color of F475W−F606W = 0.4 mag and very little spread (σ F475W−F606W = 0.03 mag), suggesting similar ages and chemical compositions.
Paper: Testing the Cosmological Principle: Astrometric Limits on Systemic Motion of Quasars at Different Cosmological Epochs
Authors: Valeri V. Makarov, Nathan J. Secrest
Figure caption: Contour maps of proper motion fields in R.A. (left) and decl. (right) coordinates fitted with 37 Zernike functions each. The values are in mas yr−1. The coordinates are in degrees. Note the direction of the R.A. axis increasing from left to right.
Paper: Testing the Cosmological Principle: Astrometric Limits on Systemic Motion of Quasars at Different Cosmological Epochs
Authors: Valeri V. Makarov, Nathan J. Secrest
Figure caption: Sky footprint of spectroscopic quasars from SDSS with valid proper motion measurements in Gaia EDR3. The red dotted line indicates the boundary of the elliptical area selected for this study.
Paper: Testing the Cosmological Principle: Astrometric Limits on Systemic Motion of Quasars at Different Cosmological Epochs
Authors: Valeri V. Makarov, Nathan J. Secrest
Figure caption: Contour maps of standard errors of the component proper motion fields in R.A. (left) and decl. (right) shown in Figure 2. The values are in mas yr−1. The coordinates are in degrees. Note the direction of the R.A. axis increasing from left to right.
Paper: Dust Resurgence in Protoplanetary Disks Due to Planetesimal–Planet Interactions
Authors: Lia Marta Bernabò, Diego Turrini, Leonardo Testi, Francesco Marzari, Danai Polychroni
Figure caption: The plots show the dust production across the radial extension of the disk (in M ⊕ per 1 au wide ring integrated over time, top row) and across time (in M ⊕ produced every 0.1 Myr spatially integrated over the whole disk, bottom row) for all runs. In both rows, the plots show the dust production for planets forming in situ (first and third panels) and for migrating planets (second and fourth panels). The first two panels in each row refer to solar-type stars, the last two to red dwarf stars.
Paper: The Combined Effects of Two-body Relaxation Processes and the Eccentric Kozai–Lidov Mechanism on the Extreme-mass-ratio Inspirals Rate
Authors: Smadar Naoz, Sanaea C. Rose, Erez Michaely, Denyz Melchor, Enrico Ramirez-Ruiz, Brenna Mockler, Jeremy D. Schnittman
Figure caption: Time evolution of an example system in the presence of different physical processes. We show, from top to bottom, a stellar-mass black hole separation around an SMBH, inclination with respect to the outer perturber, the argument of periapsis, and longitude of ascending nodes. Left side: We consider a stellar-mass black hole (m • = 10 M ⊙) orbiting an SMBH (m 1 = 107 M ⊙), at a • = 8000 au, initially with e • = 0.02, ω • = 45°, Ω• = 110°. We also consider a population of stellar-mass black holes around m 1, following a Bahcall & Wolf (1976) profile (i.e., α = 1.75). We normalize the density profile according to the m−σ relation, (see Equation (1)), which results in a two-body relaxation timescale of t relx ∼ 3.5 × 108 yr. We show the resulting orbital evolution of the stellar-mass BH in the thick red line. We also introduce a binary SMBH with mass m 2 = 109 M ⊙ set on 1 pc separation, with an eccentricity of e bin = 0.7. The evolution that includes both the two-body relaxation and the EKL from the outer orbit (as well as the GR precession on the inner orbit) is shown by the thin blue line. As depicted, this system reached extreme eccentricities induced by a combination of two-body relaxation and EKL and pushed toward the SMBH, producing a GW source. We also consider the case in which we ignore the contribution of two-body relaxation processes and consider only the EKL (+GR) in light gray. This system never reached high eccentricity to become an EMRI. On the right side, we consider the same system, only this time we arbitrarily increased the relaxation timescale to 4.3 × 1011 yr (by assuming scatter masses of 5 × 10−3 M ⊙). As depicted this system qualitatively follows the EKL (+GR) behavior.
Paper: The Combined Effects of Two-body Relaxation Processes and the Eccentric Kozai–Lidov Mechanism on the Extreme-mass-ratio Inspirals Rate
Authors: Smadar Naoz, Sanaea C. Rose, Erez Michaely, Denyz Melchor, Enrico Ramirez-Ruiz, Brenna Mockler, Jeremy D. Schnittman
Figure caption: Top panel: an illustration of the system. Middle panel: an example of the timescales in the system. We consider an SMBH of mass m 1 = 107 M ⊙ with a population of 10 M ⊙ BHs. The period of the BHs around m 1 is shown by the dashed line (labeled P •), and the associated 1pN precession is shown as the blue line, labeled t 1pN, according to Equation (3). The weak interactions between the BHs result in the two-body relaxation timescale (see Equation (5)), shown by the black line. We also consider an SMBH companion with m 2 = 109 M ⊙, at 1 pc separation (note that m 1 < m 2 in this configuration). The period of the SMBH binary is shown as the dashed line labeled P bin, and the resulting EKL timescale is the red line labeled t EKL; see Equation (2). Bottom panel: proposed alternative to quantify the relative importance of the two-body relaxation processes compared to EKL. We consider h/Δh (the relative change in angular momentum “h”), due to both two-body relaxation and EKL, where ﹩h/{\rm{\Delta }}{h}_{\mathrm{relx}}\sim \sqrt{{t}_{\mathrm{relx}}/{P}_{\bullet }}﹩ for two-body processes and h/Δh EKL ∼ t EKL/P • for EKL. See text (Section 3.1) for more details.
Paper: The Combined Effects of Two-body Relaxation Processes and the Eccentric Kozai–Lidov Mechanism on the Extreme-mass-ratio Inspirals Rate
Authors: Smadar Naoz, Sanaea C. Rose, Erez Michaely, Denyz Melchor, Enrico Ramirez-Ruiz, Brenna Mockler, Jeremy D. Schnittman
Figure caption: Monte Carlo. As a proof of concept, we consider a system composed of m 1 = 107 M ⊙ and m 2 = 109 M ⊙ with a binary separation of a bin = 1 pc and eccentricity of e bin = 0.7. We present three runs, of 1000 particles each. We consider the following processes: (top) EKL + GR, (middle) EKL + GR + two-body relaxation, (bottom) EKL + GR + two-body relaxation + GW. The initial conditions are the same at each run and are shown in gray in each panel. The red line marks the limit of crossing R crit, thus a system that ended up below the line is marked as a potential GW source, i.e., EMRI.
Paper: The Combined Effects of Two-body Relaxation Processes and the Eccentric Kozai–Lidov Mechanism on the Extreme-mass-ratio Inspirals Rate
Authors: Smadar Naoz, Sanaea C. Rose, Erez Michaely, Denyz Melchor, Enrico Ramirez-Ruiz, Brenna Mockler, Jeremy D. Schnittman
Figure caption: Scaling relation proof of concept. The top panel shows the probability density of the BHs that cross R crit and thus become a GW source, as a function of time, in each of the three simulations from Figure 3. Note that the statistical difference between the two probability densities that include the two-body relaxation is negligible. In particular, the two-sample Kolmogorov–Smirnov test does not reject the null hypothesis—that both have the same distribution—at the 20% significance level. The bottom panel shows the number of stellar-mass BHs that became GW sources as a function of time, for a range of primary masses between 105 and 108 M ⊙ (from bottom to top). In generating this estimate we have assumed a constant t EKL, constant mass ratio, and that the maximum distance for stellar-mass BHs corresponds to ϵ = 0.1; see Equation (10). We estimate the number of stellar-mass BHs using the M–σ relation (see the text for more details).
Paper: The Combined Effects of Two-body Relaxation Processes and the Eccentric Kozai–Lidov Mechanism on the Extreme-mass-ratio Inspirals Rate
Authors: Smadar Naoz, Sanaea C. Rose, Erez Michaely, Denyz Melchor, Enrico Ramirez-Ruiz, Brenna Mockler, Jeremy D. Schnittman
Figure caption: A comparison of the EMRI formation rate for a consistent number of BHs. We consider the case that includes the EKL (+GR) + two-body relaxation estimated rate from Equation (14). We compare it to the EKL (+GR)-only runs, which we consider during the burst (thin dashed line) and over sufficient replenishment time (thick dashed line). The latter is loosely estimated by assuming star formation episode and lifetime of stars to be about 50 Myr. Finally, we depict the EMRI rate for the number of BHs limited to ﹩{r}_{\max }﹩ (sphere of influence), shown as a dashed (solid) line.
Paper: Luminosities and Masses of Single Galactic Post-asymptotic Giant Branch Stars with Distances from Gaia EDR3: The Revelation of an s-process Diversity
Authors: Devika Kamath, Hans Van Winckel, Paolo Ventura, Maksym Mohorian, Bruce J. Hrivnak, Flavia Dell'Agli, Amanda Karakas
Figure caption: Positions of the Q1 and Q2 post-AGB stars in the HR diagram. The red filled circles represent the s-process enriched Q1 objects and the blue filled squares represent the non-s-process enriched Q1 objects. The red open circles represent the s-process enriched Q2 objects and the blue open squares represent the non-s-process enriched Q2 objects. The numbers represent the individual object numbers as listed in Table 1. Also shown are the available post-AGB evolutionary tracks of Miller Bertolami (2016) with Z = 0.001 (left panel) and Z = 0.01 (right panel). See text for more details.