adsabs/AstroCLIMB huggingface dataset:
Paper: First Detection of Transverse Vertical Oscillation during the Expansion of Coronal Loops
Authors: Qingmin Zhang, Chuan Li, Dong Li, Ye Qiu, Yanjie Zhang, Yiwei Ni
Figure caption: (a) Light curves of the flare in 1–8 Å, 0.5–4 Å, and 1–70 Å. (b) Normalized fluxes of the flare in 304 Å, 1600 Å, and Hα. (c) HXR light curves of the flare at various energy bands (4−300 keV). (d) Radio fluxes of the flare at 9.4 GHz, 17 GHz, and 127 MHz, respectively.
Paper: First Detection of Transverse Vertical Oscillation during the Expansion of Coronal Loops
Authors: Qingmin Zhang, Chuan Li, Dong Li, Ye Qiu, Yanjie Zhang, Yiwei Ni
Figure caption: (a) Radio dynamic spectra of the eruptive flare observed by the ALMATY station. The type III radio burst during the impulsive phase of the flare and the following type II radio burst are pointed by arrows. The horizontal dashed line is used to extract the radio flux at 127 MHz. (b) Time–distance plot of S2 in 193 Å. The northward (743 km s−1) and southward (862 km s−1) speeds of the EUV wave are labeled.
Paper: First Detection of Transverse Vertical Oscillation during the Expansion of Coronal Loops
Authors: Qingmin Zhang, Chuan Li, Dong Li, Ye Qiu, Yanjie Zhang, Yiwei Ni
Figure caption: Time evolutions of the heights (upper panel) and velocities (lower panel) of the hot channel (HC; cyan diamonds) and overlying loop (OL; orange circles). The olive dashed–dotted line indicates the onset time (05:50:30 UT) of the HC.
Paper: First Detection of Transverse Vertical Oscillation during the Expansion of Coronal Loops
Authors: Qingmin Zhang, Chuan Li, Dong Li, Ye Qiu, Yanjie Zhang, Yiwei Ni
Figure caption: Morlet wavelet transforms of the detrended light curves in Figure 7.
Paper: First Detection of Transverse Vertical Oscillation during the Expansion of Coronal Loops
Authors: Qingmin Zhang, Chuan Li, Dong Li, Ye Qiu, Yanjie Zhang, Yiwei Ni
Figure caption: Detrended light curves during the impulsive phase of the flare in EUV, HXR, and radio wavelengths.
Paper: First Detection of Transverse Vertical Oscillation during the Expansion of Coronal Loops
Authors: Qingmin Zhang, Chuan Li, Dong Li, Ye Qiu, Yanjie Zhang, Yiwei Ni
Figure caption: Time–distance plots of S1 in various EUV bands of the SDO/AIA. The trajectory of the hot channel (HC) is denoted with “+” symbols in panel (a). The trajectory of the overlying loop (OL) is denoted with “+” symbols in panel (c).
Paper: First Detection of Transverse Vertical Oscillation during the Expansion of Coronal Loops
Authors: Qingmin Zhang, Chuan Li, Dong Li, Ye Qiu, Yanjie Zhang, Yiwei Ni
Figure caption: Left panels: trajectories of ACLs (red circles) during the expansion and oscillation in 304 Å and 171 Å. The olive dashed–dotted lines represent the fitted trends. The short cyan lines mark the initial heights of ACLs before the flare. The blue lines represent the solutions of Equation (3). Right panels: results of fast Fourier transforms of the corresponding detrended trajectories. The periods of vertical oscillations are labeled.
Paper: First Detection of Transverse Vertical Oscillation during the Expansion of Coronal Loops
Authors: Qingmin Zhang, Chuan Li, Dong Li, Ye Qiu, Yanjie Zhang, Yiwei Ni
Figure caption: Top panels: a cartoon showing the collapse and oscillation of the overlying coronal loops above the flare core. Bottom panels: a cartoon showing the contraction, expansion, and vertical oscillation of ACLs close to the flare core. See text for detail.
Paper: Mixing Interstellar Clouds Surrounding the Sun
Authors: Paweł Swaczyna, Nathan A. Schwadron, Eberhard Möbius, Maciej Bzowski, Priscilla C. Frisch, Jeffrey L. Linsky, David J. McComas, Fatemeh Rahmanifard, Seth Redfield, Réka M. Winslow, Brian E. Wood, Gary P. Zank
Figure caption: Top left panel: spatial extent of the LIC (brown) and G cloud (green) projected on the sky in Galactic coordinates from Redfield & Linsky (2008). The stars within 10 pc from the Sun with identified absorption from nearby interstellar clouds are shown as filled circles (brown—LIC; green—G cloud; gray—other clouds); the crosses indicate the inflow directions of the LIC, G cloud, and pristine VLISM. Bottom left panel: color-coded cumulative distribution function of random bulk flow fluctuations inside the LIC (see text). Speed fluctuation is shown on the ordinate and angle away from the G–LIC relative flow vector on the abscissa. The observed speed and angle of the VLISM are marked as a white point with error bars. Right panels: comparison of the flow properties of the LIC and G cloud with the pristine VLISM organized by their speed in the solar frame (top to bottom): Galactic longitude, Galactic latitude, and temperature.
Paper: Mixing Interstellar Clouds Surrounding the Sun
Authors: Paweł Swaczyna, Nathan A. Schwadron, Eberhard Möbius, Maciej Bzowski, Priscilla C. Frisch, Jeffrey L. Linsky, David J. McComas, Fatemeh Rahmanifard, Seth Redfield, Réka M. Winslow, Brian E. Wood, Gary P. Zank
Figure caption: Left panel: projection of the illustrative model of the colliding LIC and G cloud forming the MICM from a direction perpendicular to the axis between the clouds. The clouds are represented as spheres with a colliding region called MICM. The orientation relative to the north Galactic pole (NGP), Galactic center (GC), and Galactic east (GE) is shown. Arrows show the relative motion of the clouds in the pristine VLISM frame. The length of the arrow representing the Sun’s velocity is reduced 10 times for illustration purposes. The line of sight toward AD Leonis traverses a significant portion of the MICM. Right panel: map in Galactic coordinates of the MICM depth as seen from the Sun, compared with the positions of AD Leonis and HD 82558. The most extended sight lines through the MICM are along the great circle (solid white line) defined by the direction along the line connecting the centers of the LIC and G cloud (white cross).
Paper: Mixing Interstellar Clouds Surrounding the Sun
Authors: Paweł Swaczyna, Nathan A. Schwadron, Eberhard Möbius, Maciej Bzowski, Priscilla C. Frisch, Jeffrey L. Linsky, David J. McComas, Fatemeh Rahmanifard, Seth Redfield, Réka M. Winslow, Brian E. Wood, Gary P. Zank
Figure caption: Comparison of flow parameter pairs from considered experiments and with the combined result. The ellipses represent uncertainty range and correlations between parameters. The STEREO result constrains only the flow ecliptic longitude. Thus, the top panels show the accepted range as bands, and the bottom panels do not show any STEREO results.
Paper: Mixing Interstellar Clouds Surrounding the Sun
Authors: Paweł Swaczyna, Nathan A. Schwadron, Eberhard Möbius, Maciej Bzowski, Priscilla C. Frisch, Jeffrey L. Linsky, David J. McComas, Fatemeh Rahmanifard, Seth Redfield, Réka M. Winslow, Brian E. Wood, Gary P. Zank
Figure caption: Temperature of the MICM obtained from two limiting cases for the mixing of the LIC and G cloud. The bands represent the 1σ uncertainty region. The MICM temperature obtained from local observations is compared to the mixing parameter obtained in this study.
Paper: Mixing Interstellar Clouds Surrounding the Sun
Authors: Paweł Swaczyna, Nathan A. Schwadron, Eberhard Möbius, Maciej Bzowski, Priscilla C. Frisch, Jeffrey L. Linsky, David J. McComas, Fatemeh Rahmanifard, Seth Redfield, Réka M. Winslow, Brian E. Wood, Gary P. Zank
Figure caption: Goodness of fit for the mixture model of the LIC and G cloud. The blue line shows the χ 2 value as a function of the mixing parameter value. The best fit is indicated by red dashed lines and the 1σ confidence interval by the green lines.
Paper: Modeling of Joint Parker Solar Probe–Metis/Solar Orbiter Observations
Authors: L. Adhikari, G. P. Zank, D. Telloni, L.-L. Zhao
Figure caption: Radial evolution of the total (2D+slab), 2D, and slab turbulence energy from the extended coronal region to the very inner heliosphere. Panels (a), (b), (c), (d), and (e) describe the outward Elsässer energy, fluctuating magnetic energy, fluctuating kinetic energy, normalized cross helicity, and normalized residual energy, respectively. The solid curve represents the 2D component, the dashed curve the slab component, and the dashed–dotted curve the 2D+slab component. The cyan triangle denotes the corresponding PSP measurement.
Paper: Modeling of Joint Parker Solar Probe–Metis/Solar Orbiter Observations
Authors: L. Adhikari, G. P. Zank, D. Telloni, L.-L. Zhao
Figure caption: Comparison between the theoretical solar wind speed and Alfvén velocity (left), and the solar wind density (right) with the observed results of the plasma parcel measured by Metis/SolO (obtained from Telloni et al. 2022b) and PSP. The solid and dashed curves are the theoretical results. The open red triangles are the observed speed and density from SolO/Metis; the cyan full triangles are the observed speed and density; and the blue full triangle is the observed Alfvén speed measured by PSP during E7.
Paper: Modeling of Joint Parker Solar Probe–Metis/Solar Orbiter Observations
Authors: L. Adhikari, G. P. Zank, D. Telloni, L.-L. Zhao
Figure caption: Radial evolution of the 2D (solid curve) and slab (dashed curve) (a) correlation lengths corresponding to the outward Elsässer energy, (b) fluctuating magnetic energy, (c) and fluctuating kinetic energy. The cyan triangle denotes the PSP measurements.
Paper: Modeling of Joint Parker Solar Probe–Metis/Solar Orbiter Observations
Authors: L. Adhikari, G. P. Zank, D. Telloni, L.-L. Zhao
Figure caption: The 2D (solid curve) and slab (dashed curve) turbulence pressure as a function of the distance. The cyan triangle is the PSP-observed turbulence pressure.
Paper: Modeling of Joint Parker Solar Probe–Metis/Solar Orbiter Observations
Authors: L. Adhikari, G. P. Zank, D. Telloni, L.-L. Zhao
Figure caption: The solar wind proton temperature as a function of the distance. The cyan triangle is the PSP-observed proton temperature.
Paper: Dynamical Unification of Tidal Disruption Events
Authors: Lars L. Thomsen, Tom M. Kwan, Lixin Dai, Samantha C. Wu, Nathaniel Roth, Enrico Ramirez-Ruiz
Figure caption: Comparison between the observed and modeled TDE blackbody luminosity, temperature, and radius. Top row (a–c): The observed quantities versus M BH for 16 optically selected TDEs (orange circles) and 7 X-ray-selected TDEs (purple triangles). (a) The observed L BB/L Edd has a clear trend with M BH. A gray line showing ﹩L=1 \% \ {\dot{M}}_{\mathrm{fb}}{c}^{2}﹩, with ﹩{\dot{M}}_{\mathrm{fb}}﹩ being the fallback rate of a 0.1 M ⊙ star, is overplotted to guide the eye. (b) X-ray TDEs have temperatures of 105 − 106 K, and optical TDEs typically have lower temperatures of a few × 104 K. (c) Optical TDEs have R BB larger than the circularization radius (red curve) or the stream self-intersection radius (green curve) (both calculated using a 0.1 M ⊙ star). X-ray TDEs can sometimes have R BB smaller than the black hole Schwarzschild radius (black line). Middle row and bottom row (d–f, g–i): The inferred quantities based on the blackbody radiation spectrum fitting the simulated spectra in the UV/optical band and X-ray band, respectively, vs. inclination angle i. Different symbols are used to mark different accretion rates: ﹩7{\dot{M}}_{\mathrm{Edd}}﹩ (blue circle), ﹩12{\dot{M}}_{\mathrm{Edd}}﹩ (green triangle), and ﹩24{\dot{M}}_{\mathrm{Edd}}﹩ (red square). Vertical lines connect the values calculated with an escaped luminosity of L bol = L Edd (smaller symbol size) and ﹩{L}_{\mathrm{bol}}=10 \% {\dot{M}}_{\mathrm{acc}}{c}^{2}﹩ (larger symbol size) to indicate possible ranges. In panels (d)–(f), TDEs with L O,BB < L X,0.3–10 keV are marked with lighter shaded symbols to indicate that they are less likely to be selected optically. Similarly, in panels (g)–(i), TDEs with L O,BB > L X,0.3–10 keV are marked with lighter shaded symbols to indicate that they are less likely to be selected by X-ray instruments. The blackbody luminosity, temperature, and radius inferred from our modeling, to the first order, reproduce the observed ones.
Paper: Dynamical Unification of Tidal Disruption Events
Authors: Lars L. Thomsen, Tom M. Kwan, Lixin Dai, Samantha C. Wu, Nathaniel Roth, Enrico Ramirez-Ruiz
Figure caption: The simulated escaping spectra of the accretion disk at different accretion rates (﹩{\dot{M}}_{\mathrm{acc}}\ =﹩ (7, 12, 24)﹩{\dot{M}}_{\mathrm{Edd}}﹩) and inclinations (i = 10°, 30°, 50°, 70°). The bolometric luminosity of the spectra L bol = L Edd for all spectra. The purple shaded region indicates the X-ray band with an energy above 0.3 keV. The orange shaded region corresponds to Swift UVOT band at 1700–6500 Å. Panels (a)–(c) show the spectral evolution with inclination angles at fixed accretion rate. All spectra change from X-ray strong to UV/optical strong as the inclination goes from the polar direction to the disk direction. Panel (d) is the same as panel (b) but only includes the spectrum at i = 10° with a blackbody spectrum fitting its X-ray continuum component and the spectrum at 70° with another blackbody spectrum fitting its UV/optical continuum component. Panels (e)–(h) show the spectral evolution with accretion rates at fixed inclinations. Three types of evolution can happen as accretion rate decreases: X-ray strong all the time (small inclination), optical/UV strong at early time and X-ray rebrightening at late time (intermediate inclination), and optical/UV strong all the time (large inclination).
Paper: Dynamical Unification of Tidal Disruption Events
Authors: Lars L. Thomsen, Tom M. Kwan, Lixin Dai, Samantha C. Wu, Nathaniel Roth, Enrico Ramirez-Ruiz
Figure caption: The 2D vertical profiles of time-ϕ-averaged gas rest-mass density ρ 0 (top panels, zoomed into the inner regions) and radiation temperature T RAD (bottom panels, whole range of the simulation box), for the three runs with different accretion rates (from left to right: ﹩{\dot{M}}_{\mathrm{acc}}=7{\dot{M}}_{\mathrm{Edd}}﹩, ﹩12{\dot{M}}_{\mathrm{Edd}}﹩, and ﹩24{\dot{M}}_{\mathrm{Edd}}﹩) in the quasi-equilibrium state. In the top panels, we show the contours of constant lab-frame radial velocity (v  r  ≡ u  r /u  t ) with white lines and show the jet regions, where the electromagnetic energy is larger than the rest-mass energy of the gas, in dark blue. In the bottom panels, the black lines indicate the electron-scattering photosphere with τ es = 1, and the red lines indicate the effective photosphere with τ eff = 1. Larger accretion rates induce larger disk/wind density and higher gas/radiation temperature, while the gas distribution and velocity structure remain rather robust against the variance in accretion rates. The sizes of photospheres generally increase as accretion rate increases.
Paper: Dynamical Unification of Tidal Disruption Events
Authors: Lars L. Thomsen, Tom M. Kwan, Lixin Dai, Samantha C. Wu, Nathaniel Roth, Enrico Ramirez-Ruiz
Figure caption: The post-peak temporal evolution of (a) the modeled TDE UV/optical luminosity, (b) temperature, (c) radius, and (d) the ratio between the UV/optical and X-ray luminosity. Different colors denote different inclination angles. The escaped radiation has luminosity L bol = L Edd for all curves. The lower axis shows the accretion rate, and the upper axis shows the corresponding time elapsed since the peak, assuming a solar-type star disrupted by a 106  M ⊙ black hole. In panels (a)–(c), we do not include the evolution i = 10°, where the event is always X-ray strong. In panel (a) the gray line shows the trend of t −5/3 to guide the eye. In panel (d) the X-ray luminosity includes only the flux in the 0.3–2 keV band for direct comparison with observations. In addition, at i = 70° the X-ray luminosities at the two higher accretion rates are negligible.
Paper: Dynamical Unification of Tidal Disruption Events
Authors: Lars L. Thomsen, Tom M. Kwan, Lixin Dai, Samantha C. Wu, Nathaniel Roth, Enrico Ramirez-Ruiz
Figure caption: The optical depth as a function of the wavelength (dashed curve) overlaid with the escaped spectra (solid curve) at two different inclinations i = 30° and i = 70° for the simulation with ﹩{\dot{M}}_{\mathrm{acc}}=12\ {\dot{M}}_{\mathrm{Edd}}﹩ and L bol = L Edd. The injected Planck spectrum at T = 106 K (brown thin curve) is also plotted to show the level of reprocessing. The photoionization edges have been marked with the green vertical lines and labeled.
Paper: Dynamical Unification of Tidal Disruption Events
Authors: Lars L. Thomsen, Tom M. Kwan, Lixin Dai, Samantha C. Wu, Nathaniel Roth, Enrico Ramirez-Ruiz
Figure caption: The simulated escaping spectra of the accretion disk at different accretion rates and inclinations, similar to Figures 2(a)–(c), except that the bolometric luminosity of the spectra ﹩{L}_{\mathrm{bol}}=10 \% \times {\dot{M}}_{\mathrm{acc}}{c}^{2}﹩.
Paper: Dynamical Unification of Tidal Disruption Events
Authors: Lars L. Thomsen, Tom M. Kwan, Lixin Dai, Samantha C. Wu, Nathaniel Roth, Enrico Ramirez-Ruiz
Figure caption: The modeled bolometric correction (L O,BB + (L X,BB)/L bol for two escaped luminosity settings. One can see that the luminosity inferred from the observations based on the assumption of blackbody radiation usually misses a large portion of the bolometric luminosity, and this problem is more severe for optical TDEs.
Paper: Multipoint Observation of the Solar Wind Interaction with Strong Lunar Magnetic Anomalies by ARTEMIS Spacecraft and Chang’E-4 Rover
Authors: Lianghai Xie, Lei Li, Aibing Zhang, Huizi Wang, Quanqi Shi, Jindong Wang, Yiteng Zhang, Bin Zhou, Yongyong Feng, Jinbin Cao, Dafei Li, Shaojin Han
Figure caption: Observing geometries of ARTEMIS and CE-4 during 01:00-08:00 UT on 31 December 2019. The central sphere represents the lunar body with color contours to show the crustal magnetic field on the lunar surface. The white circle on the lunar surface indicates the position of CE-4. The magenta circles indicate the magnetic anomalies at the Imbrium antipode, Serenitatis antipode, and Crisium antipode, respectively. The yellow and gray dots show the trajectories of ARTEMIS P1 and P1, respectively. The solid black dots indicate the time around 02:15 UT when ARMTEMIS P2 encounters the shock. The geometries are shown in the SSE coordinate, in which the solar wind flows in the opposite direction to the X-axis and the Z-axis is normal to the ecliptic plane.
Paper: Multipoint Observation of the Solar Wind Interaction with Strong Lunar Magnetic Anomalies by ARTEMIS Spacecraft and Chang’E-4 Rover
Authors: Lianghai Xie, Lei Li, Aibing Zhang, Huizi Wang, Quanqi Shi, Jindong Wang, Yiteng Zhang, Bin Zhou, Yongyong Feng, Jinbin Cao, Dafei Li, Shaojin Han
Figure caption: ENA spectra observed by CE-4. The red, green, and blue dots show the measured spectra of Case 1, Case 2, and Case 3, respectively, in which Case 1 is downstream from the magnetic anomaly and correlated with the LMM observed by ARTEMIS, while Case 2 and Case 3 are upstream from the magnetic anomaly with similar solar wind conditions to those of Case 1. The solid lines are the fitting results of the three spectra with exponential functions. The dashed lines indicate the cutoff energies, at which the ENA flux is equal to 5.4% of its initial flux at 105 eV. Texts on the right show the parameters of the three cases, in which J sw,N  is the normal component of the solar wind flux on the lunar surface; J ENA is the integrated ENA flux over the energy; E sw is the solar wind energy; and E cut is the cutoff energy.
Paper: Multipoint Observation of the Solar Wind Interaction with Strong Lunar Magnetic Anomalies by ARTEMIS Spacecraft and Chang’E-4 Rover
Authors: Lianghai Xie, Lei Li, Aibing Zhang, Huizi Wang, Quanqi Shi, Jindong Wang, Yiteng Zhang, Bin Zhou, Yongyong Feng, Jinbin Cao, Dafei Li, Shaojin Han
Figure caption: Shock observed by ARTEMIS. (a)–(c) show the ion energy spectrum, the electron energy spectrum, and the fast Fourier transform of magnetic field fluctuations measured by ARTEMIS P2; (d)–(g) show the number densities and the electron temperatures, the velocity differences, and the magnetic fields, respectively, in which subscripts of 1 and 2 indicate the measurements of P1 and P2, respectively, and the lines in different colors represent the different components in SSE coordinate. The black line in (f) shows the magnitude of velocity change between the upstream P1 measurements and the downstream P2 measurements. The gray and the black lines in (g) show the magnitudes of magnetic field measured by P1 and P2, respectively.
Paper: Multipoint Observation of the Solar Wind Interaction with Strong Lunar Magnetic Anomalies by ARTEMIS Spacecraft and Chang’E-4 Rover
Authors: Lianghai Xie, Lei Li, Aibing Zhang, Huizi Wang, Quanqi Shi, Jindong Wang, Yiteng Zhang, Bin Zhou, Yongyong Feng, Jinbin Cao, Dafei Li, Shaojin Han
Figure caption: Schematic diagram of the solar wind interaction with lunar magnetic anomalies. The green lines indicate the magnetic anomalies on the lunar surface. The dotted red lines indicate the streamlines of the solar wind. The solid gray line indicates the boundary layer near the magnetic anomalies. The solid cyan line shows the trailing shock downstream from the magnetic anomalies.
Paper: The Relation between the Mass Accretion Rate and the Disk Mass in Class I Protostars
Authors: Eleonora Fiorellino, Łukasz Tychoniec, Carlo F. Manara, Giovanni Rosotti, Simone Antoniucci, Fernando Cruz-Sáenz de Miera, Ágnes Kóspál, Brunella Nisini
Figure caption: Mass accretion rate vs. disk dust mass. The symbols are the same as in Figure 1. The solid lines represent evolutionary tracks assuming different models: purely viscous (orange), a hybrid viscous and MHD wind (brown), and dominated by MHD wind (light blue).
Paper: Immediate Origin of the Moon as a Post-impact Satellite
Authors: J. A. Kegerreis, S. Ruiz-Bonilla, V. R. Eke, R. J. Massey, T. D. Sandnes, L. F. A. Teodoro
Figure caption: Illustrative snapshots from an impact simulation where a satellite is placed directly onto a wide orbit, in this example with the lowest final eccentricity. In the middle panels, the particles that will form the satellite and inner remnant are highlighted in purple and green. The black lines show the estimated orbit. Gray and orange show the proto-Earth’s core and mantle material, respectively, and brown and yellow the same for Theia. The color luminosity varies slightly with the internal energy. The annotated time is measured from first contact, so the simulation began at −1 hr. An animation is available at http://icc.dur.ac.uk/giant_impacts/moon_wide_orbit_slice.mp4, and with the same data rendered in 3D at http://icc.dur.ac.uk/giant_impacts/moon_wide_orbit_houdini.mp4.
Paper: Immediate Origin of the Moon as a Post-impact Satellite
Authors: J. A. Kegerreis, S. Ruiz-Bonilla, V. R. Eke, R. J. Massey, T. D. Sandnes, L. F. A. Teodoro
Figure caption: The change in mass, periapsis, and orbital eccentricity of satellites that pass through a periapsis near or inside the Roche limit and retain at least 10% of their initial mass, which tends to result in a significantly wider final orbit following partial tidal stripping. Diamonds and circles show the pre- and post-periapsis satellites, respectively.
Paper: Immediate Origin of the Moon as a Post-impact Satellite
Authors: J. A. Kegerreis, S. Ruiz-Bonilla, V. R. Eke, R. J. Massey, T. D. Sandnes, L. F. A. Teodoro
Figure caption: The categorically distinct behavior of outer-satellite formation emerges consistently for resolutions above a threshold of >106.5 particles. Each panel shows a snapshot from simulations of the same scenario at the same time 3.6 hr after impact using different numbers of particles. 104 and 104.5 particles (not shown) behave similarly to 105.