adsabs/AstroCLIMB huggingface dataset:
Paper: Detection of Radio Thermal Emission from the Kuiper Belt Object (486958) Arrokoth during the New Horizons Encounter
Authors: M. K. Bird, I. R. Linscott, G. L. Tyler, O. M. Umurhan, R. A. Beyer, W. M. Grundy, C. M. Lisse, D. P. Hinson, M. Pätzold, S. A. Stern, H. A. Weaver, C. B. Olkin, L. A. Young, J. R. Spencer, K. N. Singer, J. M. Moore, G. R. Gladstone, C. C. DeBoy, M. Vincent, S. B. Porter
Figure caption: View of the sky from New Horizons during the REX CA08 observations. A black circle shows the position of the New Horizons HGA beam (3-dB beamwidth: 1.2°) when the boresight was aligned with KBO Arrokoth. The black arrow shows the position of KBO Arrokoth (moving upward in decl.). The locus of the HGA beam as it was slewed in the same direction, covering a considerable stretch of empty sky before and after the boresight was centered on the target, is shown in red. This extra leeway was required in order to accommodate a possible TOF error of up to ±180 s with respect to the predicted CA time (05:33:00 UT). Had the errors been this large, the trajectory of the KBO during CA08 would have followed one of the orange arrows (shifted by ±1° in R.A. for clarity). A short video of the CA08 viewing geometry is included in Appendix B.
Paper: Detection of Radio Thermal Emission from the Kuiper Belt Object (486958) Arrokoth during the New Horizons Encounter
Authors: M. K. Bird, I. R. Linscott, G. L. Tyler, O. M. Umurhan, R. A. Beyer, W. M. Grundy, C. M. Lisse, D. P. Hinson, M. Pätzold, S. A. Stern, H. A. Weaver, C. B. Olkin, L. A. Young, J. R. Spencer, K. N. Singer, J. M. Moore, G. R. Gladstone, C. C. DeBoy, M. Vincent, S. B. Porter
Figure caption: Synthetic silhouette representations of KBO Arrokoth showing the projected areas as viewed from New Horizons for CA03 (left panel) and CA08 (right panel). Celestial north is up. The solar illuminated fraction of the KBO was 0.997 at approach (CA03) and 0.014 at departure (CA08). The associated times and projected areas of the KBO are indicated in each panel. The KBO Arrokoth is unresolved—the projected diameter of the REX 3-dB beam at the target was ≈1090 km for CA03 and ≈315 km for CA08. Rotational changes in the projected area from Arrokoth's slow rotation (P ≈ 15.9 hr) during the short CA03 and CA06 intervals can be neglected.
Paper: Detection of Radio Thermal Emission from the Kuiper Belt Object (486958) Arrokoth during the New Horizons Encounter
Authors: M. K. Bird, I. R. Linscott, G. L. Tyler, O. M. Umurhan, R. A. Beyer, W. M. Grundy, C. M. Lisse, D. P. Hinson, M. Pätzold, S. A. Stern, H. A. Weaver, C. B. Olkin, L. A. Young, J. R. Spencer, K. N. Singer, J. M. Moore, G. R. Gladstone, C. C. DeBoy, M. Vincent, S. B. Porter
Figure caption: REX radiometry observations during CA08. Total temperature is measured during the nightside REX observations (top panel: REX A; bottom panel: REX B). The individual dots are the raw measurements taken at 1.024 s intervals. The solid red and blue lines are the same data obtained from a rolling average over 40 s. The mean and standard deviations of the plotted data are shown to the left of the curves. The vertical dashed lines indicate the interval when the KBO was within the 3-dB beam of the New Horizons HGA. The horizontal orange lines denote the calibration intervals where the KBO was greater than 1.2° from the HGA boresight. These intervals are used to define the system temperature given in each panel.
Paper: Detection of Radio Thermal Emission from the Kuiper Belt Object (486958) Arrokoth during the New Horizons Encounter
Authors: M. K. Bird, I. R. Linscott, G. L. Tyler, O. M. Umurhan, R. A. Beyer, W. M. Grundy, C. M. Lisse, D. P. Hinson, M. Pätzold, S. A. Stern, H. A. Weaver, C. B. Olkin, L. A. Young, J. R. Spencer, K. N. Singer, J. M. Moore, G. R. Gladstone, C. C. DeBoy, M. Vincent, S. B. Porter
Figure caption: Relative flux density ΔS recorded during CA08 as a function of declination.
Paper: Detection of Radio Thermal Emission from the Kuiper Belt Object (486958) Arrokoth during the New Horizons Encounter
Authors: M. K. Bird, I. R. Linscott, G. L. Tyler, O. M. Umurhan, R. A. Beyer, W. M. Grundy, C. M. Lisse, D. P. Hinson, M. Pätzold, S. A. Stern, H. A. Weaver, C. B. Olkin, L. A. Young, J. R. Spencer, K. N. Singer, J. M. Moore, G. R. Gladstone, C. C. DeBoy, M. Vincent, S. B. Porter
Figure caption: View of the sky from New Horizons during the REX CA03 observations. The New Horizons HGA boresight (red zigzag curve) was commanded to point continuously at the KBO. The large red circle denotes the size of the HGA beam (diameter: 1.2°) at the point marked “HGA boresight.” The position of KBO Arrokoth (black arrow), moving downward in decl., remained within the 3-dB HGA beam during the entire observation. The slight pointing error deviations of the boresight from the target position are due to regular small pointing corrections within the HGA dead band.
Paper: Observations and Modeling of the Opposition Surges of the Icy Moons of Saturn Based on Cassini Visual Infrared Mapping Spectrometer Data
Authors: B. J. Buratti, J. H. Hillier, P. A. Dalba, M. D. Hicks, J. A. Mosher, A. R. Hendrix, L. Abramson, N. Akhter
Figure caption: The VIMS observations at 3.60 μm compared with those of ISS at 0.35 μm and UVIS at 0.18 μm. Error bars are about twice the size of the data points. The UVIS data at 0.18 μm are from Hendrix & Buratti (2012). The UVIS Hapke model fit to the trailing side of Dione is ϖ 0 = 0.21 ± 0.02, g = −0.34, B 0 = 0.95 ± 0.15, and h = 0.5 ± 0.1 (see Hendrix & Buratti 2012, where the g is derived, and Royer & Hendrix 2014; these models are based on Hapke's earlier papers). Note that the UVIS data set is not as extensive as that of VIMS.
Paper: Observations and Modeling of the Opposition Surges of the Icy Moons of Saturn Based on Cassini Visual Infrared Mapping Spectrometer Data
Authors: B. J. Buratti, J. H. Hillier, P. A. Dalba, M. D. Hicks, J. A. Mosher, A. R. Hendrix, L. Abramson, N. Akhter
Figure caption: Hapke fits and data for Dione. The formal error bars are about the size of the data points, but more realistic data points are shown by the scatter in the data. No corrections for rotational variations were done, as all these data are from the trailing hemisphere.
Paper: Observations and Modeling of the Opposition Surges of the Icy Moons of Saturn Based on Cassini Visual Infrared Mapping Spectrometer Data
Authors: B. J. Buratti, J. H. Hillier, P. A. Dalba, M. D. Hicks, J. A. Mosher, A. R. Hendrix, L. Abramson, N. Akhter
Figure caption: The same as Figure 8, except for Rhea. Reduced data from Figures 8 and 9 along with ancillary spacecraft data are included in the supplementary package.
Paper: Observations and Modeling of the Opposition Surges of the Icy Moons of Saturn Based on Cassini Visual Infrared Mapping Spectrometer Data
Authors: B. J. Buratti, J. H. Hillier, P. A. Dalba, M. D. Hicks, J. A. Mosher, A. R. Hendrix, L. Abramson, N. Akhter
Figure caption:  B o for the shadow-hiding (B os) and coherent backscatter (B oc) effects for both Dione and Rhea. There is a slight decrease in B os with single scattering albedo, as expected. The trend for B oc is more complex and unexpected, and is discussed in the text.
Paper: Observations and Modeling of the Opposition Surges of the Icy Moons of Saturn Based on Cassini Visual Infrared Mapping Spectrometer Data
Authors: B. J. Buratti, J. H. Hillier, P. A. Dalba, M. D. Hicks, J. A. Mosher, A. R. Hendrix, L. Abramson, N. Akhter
Figure caption: Best-fit void spaces for Irvine's shadowing model for (top) Enceladus, (middle) Dione, and (bottom) Rhea. Rhea observations are from its leading side, while Dione observations are from its trailing side. Errors to the fits are ∼0.2%.
Paper: Observations and Modeling of the Opposition Surges of the Icy Moons of Saturn Based on Cassini Visual Infrared Mapping Spectrometer Data
Authors: B. J. Buratti, J. H. Hillier, P. A. Dalba, M. D. Hicks, J. A. Mosher, A. R. Hendrix, L. Abramson, N. Akhter
Figure caption: Normalized I/F extracted from the high- and low-albedo regions of Iapetus. These images were obtained at distances ranging from 3.28 to 3.43 million kilometers.
Paper: Observations and Modeling of the Opposition Surges of the Icy Moons of Saturn Based on Cassini Visual Infrared Mapping Spectrometer Data
Authors: B. J. Buratti, J. H. Hillier, P. A. Dalba, M. D. Hicks, J. A. Mosher, A. R. Hendrix, L. Abramson, N. Akhter
Figure caption: Left: opposition solar phase curves based on the shadow-hiding model of Irvine (1966). The corresponding porosities are shown in the key. Right: equivalent phase coefficients for various ranges of solar phase angles.
Paper: Observations and Modeling of the Opposition Surges of the Icy Moons of Saturn Based on Cassini Visual Infrared Mapping Spectrometer Data
Authors: B. J. Buratti, J. H. Hillier, P. A. Dalba, M. D. Hicks, J. A. Mosher, A. R. Hendrix, L. Abramson, N. Akhter
Figure caption: The coherent backscatter angular half-width (h  c ) for both Rhea and Dione. There appears to be little trend with wavelength or body until 3.6 μm. We attribute this change to the “disappearance” of small (micron-sized) particles at long wavelengths, as discussed in detail in Section 7.
Paper: Observations and Modeling of the Opposition Surges of the Icy Moons of Saturn Based on Cassini Visual Infrared Mapping Spectrometer Data
Authors: B. J. Buratti, J. H. Hillier, P. A. Dalba, M. D. Hicks, J. A. Mosher, A. R. Hendrix, L. Abramson, N. Akhter
Figure caption: The left shows a series of images of Dione going through opposition, with a minimum solar phase angle of 0.13. The right shows the ratio of the opposition surges for both bright and dark terrains, with little difference within the errors. The ISS image distances range from 1.08 to 1.02 million kilometers, with a subobserver longitude ranging from 269° to 276°.
Paper: NaCl and KCl in Io’s Atmosphere
Authors: Erin Redwing, Imke de Pater, Statia Luszcz-Cook, Katherine de Kleer, Arielle Moullet, Patricio M. Rojo
Figure caption: The Δχ 2 contour grids for all NaCl apertures analyzed in this study. Overlaid on each plot is an image of the aperture and a smaller plot with the spectral line profile for the accompanying contour grid plot, along with the best-fit output model line profile, labeled with the velocity at which the line profile is centered.
Paper: NaCl and KCl in Io’s Atmosphere
Authors: Erin Redwing, Imke de Pater, Statia Luszcz-Cook, Katherine de Kleer, Arielle Moullet, Patricio M. Rojo
Figure caption: The Δχ 2 contour grids for all KCl apertures analyzed in this study. Overlaid on each plot is an image of the aperture and a smaller plot with the spectral line profile for the accompanying contour grid plot, along with the best-fit output model line profile, labeled with the velocity at which the line profile is centered.
Paper: NaCl and KCl in Io’s Atmosphere
Authors: Erin Redwing, Imke de Pater, Statia Luszcz-Cook, Katherine de Kleer, Arielle Moullet, Patricio M. Rojo
Figure caption: Top row: (a) view of Io on 2012 October 17, when observations taken of Io showed no KCl emission; (b) view of Io on 2012 October 19, when KCl was detected; (c) same as panel (b) with observed KCl emission overlaid. Bottom row: views of Io on (d) 2018 September 2 and (e) 2018 September 11, both of which showed no KCl emission; (f) view of Io on 2018 March 20, when KCl was detected; and (g) same as panel (f) with observed KCl emission overlaid.
Paper: Miranda's Thick Regolith Indicates a Major Mantling Event from an Unknown Source
Authors: Chloe B. Beddingfield, Richard J. Cartwright
Figure caption: Timeline of Miranda’s geologic history, updated to include the major mantling event (red). Ranges of absolute age estimates of terrains were originally reported in Kirchoff et al. (2022) and Zahnle et al. (2003). The boxes represent the range of possible formation periods for Miranda’s different terrains and events. The order of events is based on both relative ages (non-bordered boxes) and absolute ages (bordered boxes; age estimates provided within the box are given in Ga). The bordered box boundaries represent the maximum and minimum ages estimates. Analysis of faults in the Global Rift System indicates that the mantling event occurred over a long period of time due to the presence of both muted and non-muted craters and scarps on the same terrains and proximal to one another. Regolith mantles some scarps within Arden but none in Elsinore, hinting that Arden Corona could be older than Elsinore Corona. This interpretation is contrary to previous relative age estimates of the coronae by Plescia (1988), Zahnle et al. (2003), and Beddingfield & Cartwright (2020), albeit their estimated absolute age ranges overlap.
Paper: Miranda's Thick Regolith Indicates a Major Mantling Event from an Unknown Source
Authors: Chloe B. Beddingfield, Richard J. Cartwright
Figure caption: Locations of impact craters analyzed (shown in a portion of image c2684626, Figure 6(c)) in a digital elevation model (DEM) created for this work. Topographic profiles for less muted craters (A–E, Figure A4) and more muted craters (1–6, Figure A5) were generated.
Paper: Miranda's Thick Regolith Indicates a Major Mantling Event from an Unknown Source
Authors: Chloe B. Beddingfield, Richard J. Cartwright
Figure caption: Annotated version of the map shown in Figure 2, presenting the locations of all images shown in Figure 6. See Figure 2 for legend.
Paper: Miranda's Thick Regolith Indicates a Major Mantling Event from an Unknown Source
Authors: Chloe B. Beddingfield, Richard J. Cartwright
Figure caption: Unannotated version of Figure 6. See Figure A2 for the specific regions covered by each image.
Paper: Miranda's Thick Regolith Indicates a Major Mantling Event from an Unknown Source
Authors: Chloe B. Beddingfield, Richard J. Cartwright
Figure caption: Topographic profiles for more muted craters 1–6 shown in Figure A3.
Paper: Miranda's Thick Regolith Indicates a Major Mantling Event from an Unknown Source
Authors: Chloe B. Beddingfield, Richard J. Cartwright
Figure caption: Topographic profiles for less muted craters A–E shown in Figure A3.
Paper: 3D Radiative-transfer Simulations of the Ejecta Plume Anticipated from DART Impact
Authors: Ludmilla Kolokolova, Jian-Yang Li, 荐扬 李, Mark van Selous, Tony Farnham, Lev Nagdimunov
Figure caption: Modeled ejecta cone for the parameters presented in Table 1. (a) The image shows the asteroid and ejecta as they will be seen by LEIA for the closest approach of LICIACube to Dimorphos, 166 s after impact; brightness is shown in logarithmic scale; sharp boundaries between brighter and fainter parts result from a rather rough grid size selected in this specific computation. (b) The radiance distribution as it changes with the projected height of the cone; the scan is made along the cone axis.
Paper: A Near-surface Temperature Model of Arrokoth
Authors: Orkan M. Umurhan, William M. Grundy, Michael K. Bird, Ross Beyer, James T. Keane, Ivan R. Linscott, Samuel Birch, Carver Bierson, Leslie A. Young, S. Alan Stern, Carey M. Lisse, Carly J. A. Howett, Silvia Protopapa, John R. Spencer, Richard P. Binzel, William B. McKinnon, Tod R. Lauer, Harold A. Weaver, Catherine B. Olkin, Kelsi N. Singer, Anne J. Verbiscer, Alex H. Parker
Figure caption: Predicted thermal inertia of amorphous ice as a function of grain size and temperature for two porosities: (top) p = 0.6, (bottom) p = 0.8 and γ = 0.37 J/m2 and ϵ = ϵ IR = 0.9. White contours highlight key ﹩{ \mathcal I }﹩ values for reference.
Paper: A Near-surface Temperature Model of Arrokoth
Authors: Orkan M. Umurhan, William M. Grundy, Michael K. Bird, Ross Beyer, James T. Keane, Ivan R. Linscott, Samuel Birch, Carver Bierson, Leslie A. Young, S. Alan Stern, Carey M. Lisse, Carly J. A. Howett, Silvia Protopapa, John R. Spencer, Richard P. Binzel, William B. McKinnon, Tod R. Lauer, Harold A. Weaver, Catherine B. Olkin, Kelsi N. Singer, Anne J. Verbiscer, Alex H. Parker
Figure caption: Diagram for simple radiative transfer calculation.
Paper: A Near-surface Temperature Model of Arrokoth
Authors: Orkan M. Umurhan, William M. Grundy, Michael K. Bird, Ross Beyer, James T. Keane, Ivan R. Linscott, Samuel Birch, Carver Bierson, Leslie A. Young, S. Alan Stern, Carey M. Lisse, Carly J. A. Howett, Silvia Protopapa, John R. Spencer, Richard P. Binzel, William B. McKinnon, Tod R. Lauer, Harold A. Weaver, Catherine B. Olkin, Kelsi N. Singer, Anne J. Verbiscer, Alex H. Parker
Figure caption: A more detailed view of encounter-day surface temperatures. Comparisons between simple theory predictions are shown: The vertical line at T ∼ 60K corresponds to the “summer” side predictions of the simple theory while the vertical line at T ∼ 12.5K corresponds to the “winter” side predictions of the same.
Paper: A Near-surface Temperature Model of Arrokoth
Authors: Orkan M. Umurhan, William M. Grundy, Michael K. Bird, Ross Beyer, James T. Keane, Ivan R. Linscott, Samuel Birch, Carver Bierson, Leslie A. Young, S. Alan Stern, Carey M. Lisse, Carly J. A. Howett, Silvia Protopapa, John R. Spencer, Richard P. Binzel, William B. McKinnon, Tod R. Lauer, Harold A. Weaver, Catherine B. Olkin, Kelsi N. Singer, Anne J. Verbiscer, Alex H. Parker
Figure caption: Minimum thermal inertia for amorphous H2O ice as a function of T and p with ϵ = 0.9. Under given conditions, this quantity implies that ﹩{ \mathcal I }\geqslant {{ \mathcal I }}_{m}(T,p)﹩. Note also this quantity is extremized at around p ≈ 0.32.
Paper: A Near-surface Temperature Model of Arrokoth
Authors: Orkan M. Umurhan, William M. Grundy, Michael K. Bird, Ross Beyer, James T. Keane, Ivan R. Linscott, Samuel Birch, Carver Bierson, Leslie A. Young, S. Alan Stern, Carey M. Lisse, Carly J. A. Howett, Silvia Protopapa, John R. Spencer, Richard P. Binzel, William B. McKinnon, Tod R. Lauer, Harold A. Weaver, Catherine B. Olkin, Kelsi N. Singer, Anne J. Verbiscer, Alex H. Parker
Figure caption: This diagram describes the shape analysis discussed in Section 3.2. The shape model depicted here is the low-order 2000 facet model analyzed in Grundy et al. (2020). However, the methods described herein are applied to the 105 facet model in Spencer et al. (2020).
Paper: T-matrix and Hapke Modeling of the Thermal Infrared Spectra of Trojan Asteroids and (944) Hidalgo: Implications for Their Regolith Particle Size and Porosity
Authors: Vanessa C. Lowry, Kerri L. Donaldson Hanna, Gen Ito, Michael S. P. Kelley, Humberto Campins, Sean Lindsay
Figure caption: The MSTM and Hapke method results of modeling Trojan and (944) Hidalgo spectra with the abundances shown in Table 5.
Paper: T-matrix and Hapke Modeling of the Thermal Infrared Spectra of Trojan Asteroids and (944) Hidalgo: Implications for Their Regolith Particle Size and Porosity
Authors: Vanessa C. Lowry, Kerri L. Donaldson Hanna, Gen Ito, Michael S. P. Kelley, Humberto Campins, Sean Lindsay
Figure caption: Summary of the full methodology outlined in Sections 2.4 and 2.5. Note that steps 4 and 5 do not use the WLS model.
Paper: T-matrix and Hapke Modeling of the Thermal Infrared Spectra of Trojan Asteroids and (944) Hidalgo: Implications for Their Regolith Particle Size and Porosity
Authors: Vanessa C. Lowry, Kerri L. Donaldson Hanna, Gen Ito, Michael S. P. Kelley, Humberto Campins, Sean Lindsay
Figure caption: Comparison between random vs. fixed orientation of light (a), a single particle size vs. a PSD (0.1–0.5 μm with a peak at 0.2 μm) (b), and a rectangular vs. spherical target (c) for modeled fayalite. Panels (a), (b), and (c) show modeled fayalite at the 0.5 μm particle size.
Paper: T-matrix and Hapke Modeling of the Thermal Infrared Spectra of Trojan Asteroids and (944) Hidalgo: Implications for Their Regolith Particle Size and Porosity
Authors: Vanessa C. Lowry, Kerri L. Donaldson Hanna, Gen Ito, Michael S. P. Kelley, Humberto Campins, Sean Lindsay
Figure caption: Asteroid (911) Agamemnon modeled using 25% by volume halite and 75% by volume fayalite (green). The modeled spectrum of 100% by volume fayalite at the 0.5 μm particle size and with a bulk porosity of 75% is shown in blue for comparison (identical to Figure 7(a)). The measured spectrum of (911) Agamemnon is shown in gray.
Paper: T-matrix and Hapke Modeling of the Thermal Infrared Spectra of Trojan Asteroids and (944) Hidalgo: Implications for Their Regolith Particle Size and Porosity
Authors: Vanessa C. Lowry, Kerri L. Donaldson Hanna, Gen Ito, Michael S. P. Kelley, Humberto Campins, Sean Lindsay
Figure caption: The WLS model fits (red lines) to Trojan and (944) Hidalgo spectra (gray lines) corresponding to Table 4.
Paper: The Geologic Impact of 16 Psyche’s Surface Temperatures
Authors: Carver J. Bierson, Linda T. Elkins-Tanton, Joseph G. O'Rourke
Figure caption: Annual temperature variations exceed 100 K over nearly all of Psyche’s surface over a wide of thermal inertia values. In the southern hemisphere, the mean temperatures are consistently lower, while the temperature variations are larger. (a) Annual mean temperature as a function of latitude and thermal inertia (Γ). (b) One profile from panel (a) for a thermal inertial of 126 tiu (same as Figure 1). This thermal inertia is a representative value chosen to show the north–south differences. (c) Difference between the local minimum surface temperature and maximum surface temperature within one Psyche orbit. (d) One profile from panel (c) for a thermal inertial of 100 tiu. For all panels, the specific heat and density are held constant (c  p  = 500 J kg−1, ρ = 2000 kg m−3), while the thermal conductivity is varied.
Paper: The Geologic Impact of 16 Psyche’s Surface Temperatures
Authors: Carver J. Bierson, Linda T. Elkins-Tanton, Joseph G. O'Rourke
Figure caption: Example of typical model output. Temperatures are shown at the equator and each pole using thermal parameters corresponding to 100 tiu (k = 0.01 W m−1 K−1, ρ = 2000 kg m−3, c  p  = 500 J kg−1). Panels (a) and (b) show temperatures with depth at the same time snapshot. Panel (b) is a zoom-in of the top 5 cm of panel (a) to emphasize the diurnal skin depth. Symbols are placed at model cell centers. Panel (c) shows the surface temperature over 1 Psyche yr. The thickness of the lines is due to the day–night temperature variations. The vertical black line corresponds to the time of panels (a) and (b).
Paper: Releasing Atmospheric Martian Dust in Sand Grain Impacts
Authors: T. Becker, J. Teiser, T. Jardiel, M. Peiteado, O. Muñoz, J. Martikainen, J. C. Gomez Martin, G. Wurm
Figure caption: Volume size distributions of ejected dust grains for the two runs with electric field applied and one run without. Overplotted is a power law fitted to the data (black solid line). The same fit, shifted by half an order of magnitude, is overplotted for the experiment without field (black dashed line). Also seen is the initial size distribution used in the sample (dust bed). It is approximated with a dashed horizontal line.
Paper: The Geologic Impact of 16 Psyche’s Surface Temperatures
Authors: Carver J. Bierson, Linda T. Elkins-Tanton, Joseph G. O'Rourke
Figure caption: Depending on the Paris law exponent, m, seasonal temperature variations may be more important than diurnal variations in crack propagation for much of Psyche’s surface. Shown are the estimated time to full crack (﹩{N}_{\mathrm{crit}}^{* }P﹩) for diurnal and annual temperature variations as a function of latitude. For this calculation, Δσ = fE αΔT, where f = 0.01. Changes in the assumed values of f, C, or a 0 would shift the timescale of both the annual and diurnal curves equally.
Paper: Releasing Atmospheric Martian Dust in Sand Grain Impacts
Authors: T. Becker, J. Teiser, T. Jardiel, M. Peiteado, O. Muñoz, J. Martikainen, J. C. Gomez Martin, G. Wurm
Figure caption: Curves of threshold friction velocities depending on grain size for different models as well as experimental results. (taken from Neakrase et al. 2016).