adsabs/AstroCLIMB huggingface dataset:
Paper: A Large Outburst, Coma Asymmetries, and the Color of Comet 243P/NEAT
Authors: Michael S. P. Kelley, Silvia Protopapa, Dennis Bodewits, Aren N. Heinze, Youssef Moulane, Quanzhi Ye, 泉志 叶, Bryce Bolin, Simon Conseil, Tony L. Farnham, Lori Feaga, Xing Gao, 兴 高, Chih-Hao Hsia, 志浩 夏, Emmanuel Jehin, Shrinivas R. Kulkarni, Russ R. Laher, 主嶺亞 良, Tim Lister, Frank J. Masci, Josiah Purdum, Bin Yang, 彬 杨
Figure caption: IRTF/SpeX spectra of comet 243P/NEAT at rh = 2.6 au, taken on 2018 December 15, 4 ± 1 days after a large outburst (circles). Also shown is an IRTF/SpeX spectrum of comet C/2013 US10 (Catalina) at 5.8 au (squares). Both spectra are normalized to 1.0 at 1.0 μm, but the Catalina spectrum has been offset by −0.2 for clarity. The Catalina spectrum is from S. Protopapa et al. (2018) and serves as an example for the 1.5 and 2.0 μm water-ice absorption features that are seen in some comets but are absent from the 243P spectrum. The icy grain model for comet Catalina from S. Protopapa et al. (2018) is also shown (solid line). Shaded regions indicate wavelengths that may be affected by strong telluric absorption. The spectrum of comet 243P is available as Data Behind the Figure.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: A Large Outburst, Coma Asymmetries, and the Color of Comet 243P/NEAT
Authors: Michael S. P. Kelley, Silvia Protopapa, Dennis Bodewits, Aren N. Heinze, Youssef Moulane, Quanzhi Ye, 泉志 叶, Bryce Bolin, Simon Conseil, Tony L. Farnham, Lori Feaga, Xing Gao, 兴 高, Chih-Hao Hsia, 志浩 夏, Emmanuel Jehin, Shrinivas R. Kulkarni, Russ R. Laher, 主嶺亞 良, Tim Lister, Frank J. Masci, Josiah Purdum, Bin Yang, 彬 杨
Figure caption: Select images of comet 243P/NEAT: (a) median ZTF pre-opposition r-band image; (b) median ZTF post-opposition r-band image; (c) mean ATLAS o-band image, 0.99 days post-outburst (resampled to 1﹩\mathop{.}\limits^{^{\prime\prime} }﹩0 pixel−1); (d) single LDT ﹩{r}^{{\prime} }﹩-band image, 4.73 days post-outburst; (e) mean LDT ﹩{r}^{{\prime} }﹩-band image, 31.73 days post-outburst. The ZTF images are generated from multiple nights of data aligned with the projected comet–Sun vector on the x-axis (see text for details). The ATLAS and LDT images are aligned with celestial north up and east to the left. Color scales for all images linearly vary from 0 to the 3σ background level, then logarithmically up to the peak pixel. Projected Sun and velocity vectors and scale bars are shown (averages for the ZTF data).
Paper: A Large Outburst, Coma Asymmetries, and the Color of Comet 243P/NEAT
Authors: Michael S. P. Kelley, Silvia Protopapa, Dennis Bodewits, Aren N. Heinze, Youssef Moulane, Quanzhi Ye, 泉志 叶, Bryce Bolin, Simon Conseil, Tony L. Farnham, Lori Feaga, Xing Gao, 兴 高, Chih-Hao Hsia, 志浩 夏, Emmanuel Jehin, Shrinivas R. Kulkarni, Russ R. Laher, 主嶺亞 良, Tim Lister, Frank J. Masci, Josiah Purdum, Bin Yang, 彬 杨
Figure caption: Variation of dust geometric cross section, G, and absolute magnitude, H, with time within a 10,000 km radius aperture during the 2021 December outburst. The dotted line corresponds to a constant dust cross section of 65 km2. Our adopted baseline coma brightness is shown as a solid black line, and the best-fit two-exponential outburst model is presented as a dashed line. The portions of the exponential that have been extrapolated beyond the fitted data are shown as dashed−dotted lines. A vertical line marks the observation time of the IRTF SpeX spectrum.
Paper: A Large Outburst, Coma Asymmetries, and the Color of Comet 243P/NEAT
Authors: Michael S. P. Kelley, Silvia Protopapa, Dennis Bodewits, Aren N. Heinze, Youssef Moulane, Quanzhi Ye, 泉志 叶, Bryce Bolin, Simon Conseil, Tony L. Farnham, Lori Feaga, Xing Gao, 兴 高, Chih-Hao Hsia, 志浩 夏, Emmanuel Jehin, Shrinivas R. Kulkarni, Russ R. Laher, 主嶺亞 良, Tim Lister, Frank J. Masci, Josiah Purdum, Bin Yang, 彬 杨
Figure caption: Inner-coma maps of comet 103P/Hartley 2 derived from Deep Impact data, oriented with the Sun to the right. A linear scale bar is shown in the lower right corner. (a) Water-ice fractional abundance by area from S. Protopapa et al. (2014). The illuminated nucleus surface has been masked. Boxes A and B from S. Protopapa et al. (2014) and an additional box C (chosen by us) are shown in all panels. (b) HRI-Vis red filter image for context, displayed as I/F (ratio of the radiance from the comet to the incident radiance from the Sun). (c) MRI spectral gradient map from the green continuum and red filters, with the color scale indicated in the figure. (d) HRI-Vis spectral gradient from the blue and red filters, using the same color scale as the MRI data.
Paper: A Large Outburst, Coma Asymmetries, and the Color of Comet 243P/NEAT
Authors: Michael S. P. Kelley, Silvia Protopapa, Dennis Bodewits, Aren N. Heinze, Youssef Moulane, Quanzhi Ye, 泉志 叶, Bryce Bolin, Simon Conseil, Tony L. Farnham, Lori Feaga, Xing Gao, 兴 高, Chih-Hao Hsia, 志浩 夏, Emmanuel Jehin, Shrinivas R. Kulkarni, Russ R. Laher, 主嶺亞 良, Tim Lister, Frank J. Masci, Josiah Purdum, Bin Yang, 彬 杨
Figure caption: Deep Impact/HRI-IR spectra of comet 103P/Hartley 2 corresponding to boxes A, B, and C in Figure 4. Also shown is the IRTF/SpeX spectrum of comet 243P/NEAT from Figure 6. Spectra are offset by a constant value for clarity. Dashed lines indicate the best-fit linear slope to the continuum at 1.45–1.8 μm and 2.2–2.4 μm. Spectra are normalized to 1.0 at 2.0 μm, based on the linear fit. Identified water-ice absorption features: 243P, none; 103P box A, none; box B, 1.5, 2.0, and 3 μm; and box C, 2.0 and 3 μm.
Paper: A Large Outburst, Coma Asymmetries, and the Color of Comet 243P/NEAT
Authors: Michael S. P. Kelley, Silvia Protopapa, Dennis Bodewits, Aren N. Heinze, Youssef Moulane, Quanzhi Ye, 泉志 叶, Bryce Bolin, Simon Conseil, Tony L. Farnham, Lori Feaga, Xing Gao, 兴 高, Chih-Hao Hsia, 志浩 夏, Emmanuel Jehin, Shrinivas R. Kulkarni, Russ R. Laher, 主嶺亞 良, Tim Lister, Frank J. Masci, Josiah Purdum, Bin Yang, 彬 杨
Figure caption: Morphology of the ZTF observations (black contours) pre-opposition (left) and post-opposition (right) compared to our example models (red contours). Contour levels are with respect to the peak pixel of the comet and spaced at factors of two intervals from 2−1 to 2−4 (pre-opposition) or 2−6 (post-opposition). The images were first smoothed with a σ = 1﹩\mathop{.}\limits^{\unicode{x02033}}﹩5 Gaussian. Image orientation is the same as in Figure 5 (Sun to the right), and a 100″ × 100″ region (∼120, 000 × 120, 000 km) is shown around each image. Panel labels correspond to the quiescent models in Table 4.
Paper: A Large Outburst, Coma Asymmetries, and the Color of Comet 243P/NEAT
Authors: Michael S. P. Kelley, Silvia Protopapa, Dennis Bodewits, Aren N. Heinze, Youssef Moulane, Quanzhi Ye, 泉志 叶, Bryce Bolin, Simon Conseil, Tony L. Farnham, Lori Feaga, Xing Gao, 兴 高, Chih-Hao Hsia, 志浩 夏, Emmanuel Jehin, Shrinivas R. Kulkarni, Russ R. Laher, 主嶺亞 良, Tim Lister, Frank J. Masci, Josiah Purdum, Bin Yang, 彬 杨
Figure caption: Photometry (circles) and model light curves (other symbols) of comet 243P/NEAT vs. time from perihelion. Labels correspond to the quiescent models in Table 4. Photometry of the small September outbursts have been removed. Most models have generally good agreement with the photometry, although they are all approximately 0.05–0.1 mag too faint after opposition (T − TP = 57 days). In addition, the isotropic model H is too bright for the pre-opposition epochs. The two lines of constant Afρ (dotted and dashed lines) are also shown to emphasize the light-curve asymmetry about opposition.
Paper: A Large Outburst, Coma Asymmetries, and the Color of Comet 243P/NEAT
Authors: Michael S. P. Kelley, Silvia Protopapa, Dennis Bodewits, Aren N. Heinze, Youssef Moulane, Quanzhi Ye, 泉志 叶, Bryce Bolin, Simon Conseil, Tony L. Farnham, Lori Feaga, Xing Gao, 兴 高, Chih-Hao Hsia, 志浩 夏, Emmanuel Jehin, Shrinivas R. Kulkarni, Russ R. Laher, 主嶺亞 良, Tim Lister, Frank J. Masci, Josiah Purdum, Bin Yang, 彬 杨
Figure caption: Images of comet 243P/NEAT and derived color, based on LDT data taken on 2018 December 16, 5 ± 1 days after a large outburst (from left to right): BC filter image, RC filter image, BC − RC color index, and regions of interest (a)–(e). North is up, east is to the left, and a scale bar is indicated. The images are at the native pixel scale of the data (0﹩\mathop{.}\limits^{^{\prime\prime} }﹩24 pixel−1), but the color map has been 3 × 3 binned. Five square regions of interest are shown, centered at the following distances to the nucleus: (a) 0 km, (b), 15,000 km, (c) 20,000 km, (d) 33,000 km, and (e) 25,000 km.
Paper: A Large Outburst, Coma Asymmetries, and the Color of Comet 243P/NEAT
Authors: Michael S. P. Kelley, Silvia Protopapa, Dennis Bodewits, Aren N. Heinze, Youssef Moulane, Quanzhi Ye, 泉志 叶, Bryce Bolin, Simon Conseil, Tony L. Farnham, Lori Feaga, Xing Gao, 兴 高, Chih-Hao Hsia, 志浩 夏, Emmanuel Jehin, Shrinivas R. Kulkarni, Russ R. Laher, 主嶺亞 良, Tim Lister, Frank J. Masci, Josiah Purdum, Bin Yang, 彬 杨
Figure caption: Photometry of comet 243P/NEAT showing a small outburst near 15 days after perihelion. A slope of −0.024 mag day−1 has been removed from the data. A best-fit exponential curve with a fixed peak time of 2018 September 10 at 12:05 UTC, an amplitude of −0.28 ± 0.04 mag, and a timescale of 8.6 ± 2.1 days is shown. A second event may have occurred near T − TP = 28 days.
Paper: A Large Outburst, Coma Asymmetries, and the Color of Comet 243P/NEAT
Authors: Michael S. P. Kelley, Silvia Protopapa, Dennis Bodewits, Aren N. Heinze, Youssef Moulane, Quanzhi Ye, 泉志 叶, Bryce Bolin, Simon Conseil, Tony L. Farnham, Lori Feaga, Xing Gao, 兴 高, Chih-Hao Hsia, 志浩 夏, Emmanuel Jehin, Shrinivas R. Kulkarni, Russ R. Laher, 主嶺亞 良, Tim Lister, Frank J. Masci, Josiah Purdum, Bin Yang, 彬 杨
Figure caption: Morphology of the LDT image taken on 2018 December 16 and example outburst models. The data and models are shown as black and red isophotal contours, respectively, spaced at factor of two intervals from 2−3 to 2−8. Panel labels correspond to the outburst models in Table 4. All models use s1 = 60 m s−1, 0.1 μm<a < 1 mm, and dn/da ∝ a−3.5, unless noted. The images were smoothed with a ﹩\sigma =0\mathop{.}\limits^{^{\prime\prime} }5﹩ Gaussian kernel. Image scale and orientation are indicated on the right. Each row signifies the variation of a different parameter: models A–D vary ejection speed, models E–G vary the opening angle of a sunward cone, models H–J vary the power-law slope on the grain size distribution, and models K–N vary grain size range. Model M better represents the compactness of the ejecta and the flattened sunward distribution (see Section 5.3.2 for a discussion), although additional asymmetries and perhaps the addition of the quiescent activity may be necessary to account for the elongation of the isophotes toward PA ∼ 90°.
Paper: A Large Outburst, Coma Asymmetries, and the Color of Comet 243P/NEAT
Authors: Michael S. P. Kelley, Silvia Protopapa, Dennis Bodewits, Aren N. Heinze, Youssef Moulane, Quanzhi Ye, 泉志 叶, Bryce Bolin, Simon Conseil, Tony L. Farnham, Lori Feaga, Xing Gao, 兴 高, Chih-Hao Hsia, 志浩 夏, Emmanuel Jehin, Shrinivas R. Kulkarni, Russ R. Laher, 主嶺亞 良, Tim Lister, Frank J. Masci, Josiah Purdum, Bin Yang, 彬 杨
Figure caption: Dust production scaling function (Q, dimensionless) that produces an ejecta morphology in best agreement with our first LDT image. The production rate follows ﹩{\cos }^{2}(\theta /2)﹩, where θ is measured from R.A., decl. = (140°, 30°), shown here as the vector ﹩\hat{n}﹩. The comet−Sun (⊙) and comet−observer (⊕) vectors are also shown. Left: the view from Earth (﹩\hat{y}﹩ is equatorial north, ﹩\hat{x}﹩ is west). Right: top-down view of the Sun−comet plane (﹩\hat{y}﹩ is the Sun−comet unit vector, ﹩\hat{x}﹩ is perpendicular to the Sun direction in the comet’s orbital plane).
Paper: A Large Outburst, Coma Asymmetries, and the Color of Comet 243P/NEAT
Authors: Michael S. P. Kelley, Silvia Protopapa, Dennis Bodewits, Aren N. Heinze, Youssef Moulane, Quanzhi Ye, 泉志 叶, Bryce Bolin, Simon Conseil, Tony L. Farnham, Lori Feaga, Xing Gao, 兴 高, Chih-Hao Hsia, 志浩 夏, Emmanuel Jehin, Shrinivas R. Kulkarni, Russ R. Laher, 主嶺亞 良, Tim Lister, Frank J. Masci, Josiah Purdum, Bin Yang, 彬 杨
Figure caption: Same as Figure 10, but including model outburst light curves. Triangles represent a subset of dynamical models tested (Table 4). Our adopted baseline coma brightness is shown as a solid black line, and the best-fit two-exponential outburst model is presented as a dashed line. Model M best represents all aspects of the data, but model N is still a fair representation of the light curve.
Paper: A Large Outburst, Coma Asymmetries, and the Color of Comet 243P/NEAT
Authors: Michael S. P. Kelley, Silvia Protopapa, Dennis Bodewits, Aren N. Heinze, Youssef Moulane, Quanzhi Ye, 泉志 叶, Bryce Bolin, Simon Conseil, Tony L. Farnham, Lori Feaga, Xing Gao, 兴 高, Chih-Hao Hsia, 志浩 夏, Emmanuel Jehin, Shrinivas R. Kulkarni, Russ R. Laher, 主嶺亞 良, Tim Lister, Frank J. Masci, Josiah Purdum, Bin Yang, 彬 杨
Figure caption: Water-ice grain lifetimes, i.e., time to complete sublimation, vs. grain size for pure and dirty grains (0.0%, 0.2%, and 0.5% amorphous carbon by volume). Lines of constant heliocentric distance are shown as solid lines from 0.5 to 8.0 au in 0.5 au steps. A dashed line indicates grain lifetimes specific to the circumstances of the 243P/NEAT outburst of 2021 December at 2.55 au from the Sun. A horizontal bar indicates the post-outburst time for our near-infrared spectrum of 243P. Grains on the 243P line with lifetimes below the shaded region would have sublimated away before being observed.
Paper: Spectral Properties of Ilmenite, Hematite, and Spinel: Implications for Upcoming Lunar Exploration Missions
Authors: Alex Camon, Myriam Lemelin
Figure caption: Spectra of (a) ilmenite, (b) hematite, (c) spinel, and (d) LHS-1 simulant as a function of the emission angle acquired with an incidence angle of 30° and a maximum grain size of 20 μm. The shades of red correspond to positive emission angles when the sensor is placed on the same side as the light source on the goniometer (backscattering). The shades of blue correspond to negative emission angles when the sensor is placed on the opposite side of the light source (forward scattering). The lighter the color, the closer the emission angle is to 0° (i.e., the closer the sensor is to the nadir). The emission angle at 0° is distinguished by its purple color. Measurements of ilmenite spectra at a phase angle of 10° were not included, due to limitations in the setup.
Paper: Spectral Properties of Ilmenite, Hematite, and Spinel: Implications for Upcoming Lunar Exploration Missions
Authors: Alex Camon, Myriam Lemelin
Figure caption: Spectra of (a) ilmenite, (b) hematite, (c) spinel, and (d) LHS-1 presented as a function of grain size (μm) under a fixed viewing geometry (i = 30°, e = 0°). Dotted lines represent the main mineral absorption band.
Paper: Spectral Properties of Ilmenite, Hematite, and Spinel: Implications for Upcoming Lunar Exploration Missions
Authors: Alex Camon, Myriam Lemelin
Figure caption: Bidirectional reflectance is presented for (a) ilmenite, (b) hematite, (c) spinel, and (d) LHS-1 with grain size <20 μm. Each graph illustrates reflectance intensity as a function of emission angle across multiple spectral bands and with an incidence angle of 0°. Trend lines are fourth-degree polynomial curves.
Paper: Spectral Properties of Ilmenite, Hematite, and Spinel: Implications for Upcoming Lunar Exploration Missions
Authors: Alex Camon, Myriam Lemelin
Figure caption: Diagram of the installation of the ASD FieldSpec 4 high-resolution NG spectrometer on the goniometer.
Paper: Spectral Properties of Ilmenite, Hematite, and Spinel: Implications for Upcoming Lunar Exploration Missions
Authors: Alex Camon, Myriam Lemelin
Figure caption: Comparison of measured and modeled spectra (selected based on the minimum RMSE value) for (a) ilmenite/LHS with 15 wt% mineral, (b) hematite/LHS with 42 wt% mineral, and (c) spinel/LHS with 24 wt% mineral mixtures with bulk grain sizes (<250 μm), under a fixed viewing geometry (i = 30°, e = 0°). Modeled spectra are shown with dashed lines, while measured spectra are shown with solid lines. Dark colors represent continuum-removed spectra, and light colors represent reflectance spectra. Vertical offsets were applied for clarity and are indicated in the graph.
Paper: Spectral Properties of Ilmenite, Hematite, and Spinel: Implications for Upcoming Lunar Exploration Missions
Authors: Alex Camon, Myriam Lemelin
Figure caption: Mixed spectra of (a) ilmenite, (b) hematite, and (c) spinel with LHS-1, varying in mineral abundance. These spectra were collected using an ASD FieldSpec 4 high-resolution NG spectrometer under fixed viewing conditions (e = 0°, i = 30°). The 0 wt% spectrum represents pure LHS-1, while 100 wt% represents the pure mineral. The pure samples have a grain size of 20 μm and were measured under the same acquisition angles as the mixtures. Vertical offsets were applied for better visualization and are indicated in the graph. Dotted lines highlight mineral absorption band.
Paper: Spectral Properties of Ilmenite, Hematite, and Spinel: Implications for Upcoming Lunar Exploration Missions
Authors: Alex Camon, Myriam Lemelin
Figure caption: Band ratio and band parameter results for (a) ilmenite, (b) hematite, and (c) Mg spinel. We computed band ratios and band parameters on the pure LHS-1 spectrum (0 wt% target mineral) to assess a detection threshold. Since LHS-1 contains 0.4 wt% ilmenite, the first band ratio value was adjusted to start at 0.4 instead of 0.
Paper: Spectral Properties of Ilmenite, Hematite, and Spinel: Implications for Upcoming Lunar Exploration Missions
Authors: Alex Camon, Myriam Lemelin
Figure caption: MIR spectral mixtures of (a) ilmenite and LHS, (b) hematite and LHS, and (c) spinel and LHS, based on mineral abundance, measured under a fixed viewing geometry (phase angle = 0°).
Paper: Spectral Properties of Ilmenite, Hematite, and Spinel: Implications for Upcoming Lunar Exploration Missions
Authors: Alex Camon, Myriam Lemelin
Figure caption: MIR spectra of ilmenite (top left), hematite (top right), spinel (bottom left), and LHS (bottom right) with varying grain sizes, all measured under a fixed viewing geometry (phase angle = 0°).
Paper: JWST Spectroscopy of (142) Polana: Connection to NEAs (101955) Bennu and (162173) Ryugu
Authors: Anicia Arredondo, Tracy M. Becker, Maggie M. McAdam, Andrew S. Rivkin, Stephanie Jarmak, Ian Wong
Figure caption: Left: extracted flux from the two NIRSpec grating-filter combinations. The extracted flux of the solar analog star scaled to the flux of the asteroid is shown in yellow. Right: extracted flux from the 12 MIRI subchannels. The best-fit NEATM model is shown in gray.
Paper: JWST Spectroscopy of (142) Polana: Connection to NEAs (101955) Bennu and (162173) Ryugu
Authors: Anicia Arredondo, Tracy M. Becker, Maggie M. McAdam, Andrew S. Rivkin, Stephanie Jarmak, Ian Wong
Figure caption: Hydrogen content of asteroids from A. S. Rivkin et al. (2025) determined by various techniques. Polana results added from this study. Shaded regions show the range of H wt % for carbonaceous chondrites from L. G. Vacher et al. (2020). Polana is similar to Bennu and Ryugu and unlike the CI and CM chondrites.
Paper: JWST Spectroscopy of (142) Polana: Connection to NEAs (101955) Bennu and (162173) Ryugu
Authors: Anicia Arredondo, Tracy M. Becker, Maggie M. McAdam, Andrew S. Rivkin, Stephanie Jarmak, Ian Wong
Figure caption: Comparison of JWST spectra of Polana, OSIRIS-REx spectra of Bennu from V. E. Hamilton et al. (2021, 2022), and laboratory spectrum of the returned sample from D. S. Lauretta et al. (2024). Gray lines indicate the positions of features identified in the Bennu spectra at 2.7, 3.4, and 3.8 μm in the left panel and 7.04, 9.17, 18.0, and 18.93 μm in the right panel. The Polana spectrum is normalized to unity at 2.4 μm. The shaded regions indicate error. Data without offsets are presented in Figure 8.
Paper: JWST Spectroscopy of (142) Polana: Connection to NEAs (101955) Bennu and (162173) Ryugu
Authors: Anicia Arredondo, Tracy M. Becker, Maggie M. McAdam, Andrew S. Rivkin, Stephanie Jarmak, Ian Wong
Figure caption: MIRI spectrum of Polana compared to Spitzer spectra of (45) Eugenia and (762) Pulcova and ISO and SOFIA spectrum of (1) Ceres. Spectral features and the location of the instrumental artifact are identified with arrows. The shaded regions indicate error.
Paper: JWST Spectroscopy of (142) Polana: Connection to NEAs (101955) Bennu and (162173) Ryugu
Authors: Anicia Arredondo, Tracy M. Becker, Maggie M. McAdam, Andrew S. Rivkin, Stephanie Jarmak, Ian Wong
Figure caption: Continuum-removed reflectance showing shallow features at 3.45 μm (middle) and 3.89 μm (right). The left panel shows the points that were used to fit a 1D polynomial to the normalized reflectance spectrum in Figure 2. The shaded purple region indicates error.
Paper: JWST Spectroscopy of (142) Polana: Connection to NEAs (101955) Bennu and (162173) Ryugu
Authors: Anicia Arredondo, Tracy M. Becker, Maggie M. McAdam, Andrew S. Rivkin, Stephanie Jarmak, Ian Wong
Figure caption: NIRSpec spectrum of Polana (purple) compared to ground-based data from N. Pinilla-Alonso et al. (2016; pink). Spectral features are identified with arrows. The shaded purple region indicates error. Both spectra are normalized to unity at 2.4 μm.
Paper: JWST Spectroscopy of (142) Polana: Connection to NEAs (101955) Bennu and (162173) Ryugu
Authors: Anicia Arredondo, Tracy M. Becker, Maggie M. McAdam, Andrew S. Rivkin, Stephanie Jarmak, Ian Wong
Figure caption: NIR spectrum of Polana compared to Ryugu from the NIRS3 instrument (K. Kitazato et al. 2019) and from returned samples (T. Yada et al. 2022). Gray lines indicate the positions of features identified in the Ryugu spectra at 2.7, 3.1, and 3.4 μm. Data without offsets are presented in Figure 8.
Paper: JWST Spectroscopy of (142) Polana: Connection to NEAs (101955) Bennu and (162173) Ryugu
Authors: Anicia Arredondo, Tracy M. Becker, Maggie M. McAdam, Andrew S. Rivkin, Stephanie Jarmak, Ian Wong
Figure caption: Comparison of NIRSpec Polana data to Bennu and Ryugu data without reflectance offsets. All spectra have been normalized to unity at 2.4 μm.
Paper: Structure and Melting of Fe, MgO, SiO2, and MgSiO3 in Planets: Database, Inversion, and Phase Diagram
Authors: Junjie Dong, 俊杰 董, Gabriel-Darius Mardaru, Paul D. Asimow, Lars P. Stixrude, Rebecca A. Fischer
Figure caption: P–T phase diagram of MgO up to 5000 GPa. MgO is the magnesium end-member of ferropericlase, a key mineral phase that is abundant in Earth’s mantle and likely present in the mantle of super-Earths. Its B1–B2 phase transition occurs at 400–500 GPa in the interiors of super-Earths, and a B1–B2–liquid triple point is located around 310 GPa and 10,000 K. For comparison, phase boundaries from A. Zerr & R. Boehler (1994; dashed–dotted line), L. Zhang & Y. Fei (2008; dotted line), and T. Kimura et al. (2017; dashed line) are also shown. Data points contributed by static compression experiments, dynamic compression experiments, and computer simulations are marked with circles, triangles, and squares, respectively, and coded with different colors based on the stable phase observed at that P–T condition.
Paper: Structure and Melting of Fe, MgO, SiO2, and MgSiO3 in Planets: Database, Inversion, and Phase Diagram
Authors: Junjie Dong, 俊杰 董, Gabriel-Darius Mardaru, Paul D. Asimow, Lars P. Stixrude, Rebecca A. Fischer
Figure caption: Global inversion of the Fe phase diagram (a) with and (b) without potential outliers. Discrepancies in the high-pressure melting curve of Fe have led to ongoing debate over its P–T phase diagram. Our inversion identifies five potential outlier data sets (blue circles in panel (a)), which report systematically lower melting temperatures. Excluding these data sets (panel (b)) results in a melting curve that aligns more closely with thermodynamic models (T. Komabayashi 2014; P. I. Dorogokupets et al. 2017) and eliminates an unphysical cusp near the γ–ϵ–liquid triple point.