adsabs/AstroCLIMB huggingface dataset:
Paper: SRGeJ045359.9+622444: A 55 Minute Period Eclipsing AM Canum Venaticorum Star Discovered from a Joint SRG/eROSITA + ZTF Search
Authors: Antonio C. Rodriguez, Ilkham Galiullin, Marat Gilfanov, Shrinivas R. Kulkarni, Irek Khamitov, Ilfan Bikmaev, Jan van Roestel, Lev Yungelson, Kareem El-Badry, Rashid Sunayev, Thomas A. Prince, Mikhail Buntov, Ilaria Caiazzo, Andrew Drake, Mark Gorbachev, Matthew J. Graham, Rustam Gumerov, Eldar Irtuganov, Russ R. Laher, Frank J. Masci, Pavel Medvedev, Josiah Purdum, Nail Sakhibullin, Alexander Sklyanov, Roger Smith, Paula Szkody, Zachary P. Vanderbosch
Figure caption: ZTF light curves of SRGeJ0453 on g, r filters: long-term (top), and folded at the 55.08 minute orbital period (bottom). No significant outbursts are seen over the ≈5 yr long baseline.
Paper: SRGeJ045359.9+622444: A 55 Minute Period Eclipsing AM Canum Venaticorum Star Discovered from a Joint SRG/eROSITA + ZTF Search
Authors: Antonio C. Rodriguez, Ilkham Galiullin, Marat Gilfanov, Shrinivas R. Kulkarni, Irek Khamitov, Ilfan Bikmaev, Jan van Roestel, Lev Yungelson, Kareem El-Badry, Rashid Sunayev, Thomas A. Prince, Mikhail Buntov, Ilaria Caiazzo, Andrew Drake, Mark Gorbachev, Matthew J. Graham, Rustam Gumerov, Eldar Irtuganov, Russ R. Laher, Frank J. Masci, Pavel Medvedev, Josiah Purdum, Nail Sakhibullin, Alexander Sklyanov, Roger Smith, Paula Szkody, Zachary P. Vanderbosch
Figure caption: Optical light curve of SRGeJ0453 observed by RTT-150, where the axes are the G magnitude vs. the time from the start of the observations in units of minutes (top—the first night of observations; and bottom—the second night of observations).
Paper: SRGeJ045359.9+622444: A 55 Minute Period Eclipsing AM Canum Venaticorum Star Discovered from a Joint SRG/eROSITA + ZTF Search
Authors: Antonio C. Rodriguez, Ilkham Galiullin, Marat Gilfanov, Shrinivas R. Kulkarni, Irek Khamitov, Ilfan Bikmaev, Jan van Roestel, Lev Yungelson, Kareem El-Badry, Rashid Sunayev, Thomas A. Prince, Mikhail Buntov, Ilaria Caiazzo, Andrew Drake, Mark Gorbachev, Matthew J. Graham, Rustam Gumerov, Eldar Irtuganov, Russ R. Laher, Frank J. Masci, Pavel Medvedev, Josiah Purdum, Nail Sakhibullin, Alexander Sklyanov, Roger Smith, Paula Szkody, Zachary P. Vanderbosch
Figure caption: The X-ray spectrum of SRGeJ0453 over the data of four SRG/eROSITA all-sky surveys (top panel). A red line shows the best-fit power-law model from Table 3. The bottom panel shows the residuals (ratio of the data divided by the model) in each energy channel.
Paper: SRGeJ045359.9+622444: A 55 Minute Period Eclipsing AM Canum Venaticorum Star Discovered from a Joint SRG/eROSITA + ZTF Search
Authors: Antonio C. Rodriguez, Ilkham Galiullin, Marat Gilfanov, Shrinivas R. Kulkarni, Irek Khamitov, Ilfan Bikmaev, Jan van Roestel, Lev Yungelson, Kareem El-Badry, Rashid Sunayev, Thomas A. Prince, Mikhail Buntov, Ilaria Caiazzo, Andrew Drake, Mark Gorbachev, Matthew J. Graham, Rustam Gumerov, Eldar Irtuganov, Russ R. Laher, Frank J. Masci, Pavel Medvedev, Josiah Purdum, Nail Sakhibullin, Alexander Sklyanov, Roger Smith, Paula Szkody, Zachary P. Vanderbosch
Figure caption: Phase-resolved spectra of He I 6678.2 Å  (above) and 7065.2 Å  (below) with resulting MCMC parameter estimates of the radial velocities. The spectrum at phase 0.97 is clearly asymmetric in both lines, confirming that the disk is eclipsed by the donor at the orbital phase. The MCMC parameter estimates are therefore done without the spectrum at that orbital phase and result in a good fit that would not be possible if that point were included. The in-eclipse RV measurement is shown in gray to indicate that it is not used in the MCMC analysis.
Paper: SRGeJ045359.9+622444: A 55 Minute Period Eclipsing AM Canum Venaticorum Star Discovered from a Joint SRG/eROSITA + ZTF Search
Authors: Antonio C. Rodriguez, Ilkham Galiullin, Marat Gilfanov, Shrinivas R. Kulkarni, Irek Khamitov, Ilfan Bikmaev, Jan van Roestel, Lev Yungelson, Kareem El-Badry, Rashid Sunayev, Thomas A. Prince, Mikhail Buntov, Ilaria Caiazzo, Andrew Drake, Mark Gorbachev, Matthew J. Graham, Rustam Gumerov, Eldar Irtuganov, Russ R. Laher, Frank J. Masci, Pavel Medvedev, Josiah Purdum, Nail Sakhibullin, Alexander Sklyanov, Roger Smith, Paula Szkody, Zachary P. Vanderbosch
Figure caption: PHOEBE modeling of the eclipsing AM CVn system allows us to constrain the model parameters of SRGeJ0453. Left: CHIMERA r- (red) and g-band (blue) light curves plotted alongside the best-fitting PHOEBE models. Right: Goodness-of-fit (χ 2/dof) for all PHOEBE models. In black, we show the model parameters where χ 2/dof < 2.3, indicating a good fit to the data.
Paper: SRGeJ045359.9+622444: A 55 Minute Period Eclipsing AM Canum Venaticorum Star Discovered from a Joint SRG/eROSITA + ZTF Search
Authors: Antonio C. Rodriguez, Ilkham Galiullin, Marat Gilfanov, Shrinivas R. Kulkarni, Irek Khamitov, Ilfan Bikmaev, Jan van Roestel, Lev Yungelson, Kareem El-Badry, Rashid Sunayev, Thomas A. Prince, Mikhail Buntov, Ilaria Caiazzo, Andrew Drake, Mark Gorbachev, Matthew J. Graham, Rustam Gumerov, Eldar Irtuganov, Russ R. Laher, Frank J. Masci, Pavel Medvedev, Josiah Purdum, Nail Sakhibullin, Alexander Sklyanov, Roger Smith, Paula Szkody, Zachary P. Vanderbosch
Figure caption: Doppler tomogram and trailed spectra for He I 5876.5 Å reveals a disk with at least one prominent bright spot. The Doppler tomogram of He I 6678.2 Å  suggests there could be a second bright spot, but this could be an artifact due to a possible cosmic ray in one of the spectra.
Paper: SRGeJ045359.9+622444: A 55 Minute Period Eclipsing AM Canum Venaticorum Star Discovered from a Joint SRG/eROSITA + ZTF Search
Authors: Antonio C. Rodriguez, Ilkham Galiullin, Marat Gilfanov, Shrinivas R. Kulkarni, Irek Khamitov, Ilfan Bikmaev, Jan van Roestel, Lev Yungelson, Kareem El-Badry, Rashid Sunayev, Thomas A. Prince, Mikhail Buntov, Ilaria Caiazzo, Andrew Drake, Mark Gorbachev, Matthew J. Graham, Rustam Gumerov, Eldar Irtuganov, Russ R. Laher, Frank J. Masci, Pavel Medvedev, Josiah Purdum, Nail Sakhibullin, Alexander Sklyanov, Roger Smith, Paula Szkody, Zachary P. Vanderbosch
Figure caption: Phase-resolved spectra of He I 4387.9 Å  with resulting MCMC parameter estimates of the radial velocities. The He I 4387.9 Å  line is poorly fit due to the strong central absorption feature, which affects the final parameter estimates. Stronger He I Å  lines, however, are not affected by a low signal-to-noise ratio or strong absorption (see Figure 16).
Paper: SRGeJ045359.9+622444: A 55 Minute Period Eclipsing AM Canum Venaticorum Star Discovered from a Joint SRG/eROSITA + ZTF Search
Authors: Antonio C. Rodriguez, Ilkham Galiullin, Marat Gilfanov, Shrinivas R. Kulkarni, Irek Khamitov, Ilfan Bikmaev, Jan van Roestel, Lev Yungelson, Kareem El-Badry, Rashid Sunayev, Thomas A. Prince, Mikhail Buntov, Ilaria Caiazzo, Andrew Drake, Mark Gorbachev, Matthew J. Graham, Rustam Gumerov, Eldar Irtuganov, Russ R. Laher, Frank J. Masci, Pavel Medvedev, Josiah Purdum, Nail Sakhibullin, Alexander Sklyanov, Roger Smith, Paula Szkody, Zachary P. Vanderbosch
Figure caption: Doppler tomograms and trailed spectra of He I 7065.2 Å  reveal a disk with at least one prominent bright spot (upper panel). The He II 4685.7 Å  Doppler tomogram (lower panel) shows the line to originate near the system center of mass, indicating it is the “central spike” seen in other AM CVn systems.
Paper: SRGeJ045359.9+622444: A 55 Minute Period Eclipsing AM Canum Venaticorum Star Discovered from a Joint SRG/eROSITA + ZTF Search
Authors: Antonio C. Rodriguez, Ilkham Galiullin, Marat Gilfanov, Shrinivas R. Kulkarni, Irek Khamitov, Ilfan Bikmaev, Jan van Roestel, Lev Yungelson, Kareem El-Badry, Rashid Sunayev, Thomas A. Prince, Mikhail Buntov, Ilaria Caiazzo, Andrew Drake, Mark Gorbachev, Matthew J. Graham, Rustam Gumerov, Eldar Irtuganov, Russ R. Laher, Frank J. Masci, Pavel Medvedev, Josiah Purdum, Nail Sakhibullin, Alexander Sklyanov, Roger Smith, Paula Szkody, Zachary P. Vanderbosch
Figure caption: Position of SRGeJ0453 in the 100 pc Gaia Hertzsprung–Russell diagram alongside previously known AM CVn systems with a significant Gaia parallax (parallax_over_error > 3). The nonoutbursting population occupies distinct portions of the phase space.
Paper: SRGeJ045359.9+622444: A 55 Minute Period Eclipsing AM Canum Venaticorum Star Discovered from a Joint SRG/eROSITA + ZTF Search
Authors: Antonio C. Rodriguez, Ilkham Galiullin, Marat Gilfanov, Shrinivas R. Kulkarni, Irek Khamitov, Ilfan Bikmaev, Jan van Roestel, Lev Yungelson, Kareem El-Badry, Rashid Sunayev, Thomas A. Prince, Mikhail Buntov, Ilaria Caiazzo, Andrew Drake, Mark Gorbachev, Matthew J. Graham, Rustam Gumerov, Eldar Irtuganov, Russ R. Laher, Frank J. Masci, Pavel Medvedev, Josiah Purdum, Nail Sakhibullin, Alexander Sklyanov, Roger Smith, Paula Szkody, Zachary P. Vanderbosch
Figure caption: RV measurements of the He II 4686 Å line show a systemic offset (dotted line; γ = 192 km s−1) and an RV amplitude of K = 9 ± 7 km s−1 (3σ confidence limit shown in gray). This low amplitude suggests that the emission originates near the binary center of mass and therefore the surface of the WD. For more details, see Section 4.1.2.
Paper: SRGeJ045359.9+622444: A 55 Minute Period Eclipsing AM Canum Venaticorum Star Discovered from a Joint SRG/eROSITA + ZTF Search
Authors: Antonio C. Rodriguez, Ilkham Galiullin, Marat Gilfanov, Shrinivas R. Kulkarni, Irek Khamitov, Ilfan Bikmaev, Jan van Roestel, Lev Yungelson, Kareem El-Badry, Rashid Sunayev, Thomas A. Prince, Mikhail Buntov, Ilaria Caiazzo, Andrew Drake, Mark Gorbachev, Matthew J. Graham, Rustam Gumerov, Eldar Irtuganov, Russ R. Laher, Frank J. Masci, Pavel Medvedev, Josiah Purdum, Nail Sakhibullin, Alexander Sklyanov, Roger Smith, Paula Szkody, Zachary P. Vanderbosch
Figure caption: Period determination with two epochs of RTT-150 data comparison. Blue circles correspond to the 2023 January 19 data, and red circles correspond to the 2023 January 20 data, with Gaussian fits as solid lines.
Paper: SRGeJ045359.9+622444: A 55 Minute Period Eclipsing AM Canum Venaticorum Star Discovered from a Joint SRG/eROSITA + ZTF Search
Authors: Antonio C. Rodriguez, Ilkham Galiullin, Marat Gilfanov, Shrinivas R. Kulkarni, Irek Khamitov, Ilfan Bikmaev, Jan van Roestel, Lev Yungelson, Kareem El-Badry, Rashid Sunayev, Thomas A. Prince, Mikhail Buntov, Ilaria Caiazzo, Andrew Drake, Mark Gorbachev, Matthew J. Graham, Rustam Gumerov, Eldar Irtuganov, Russ R. Laher, Frank J. Masci, Pavel Medvedev, Josiah Purdum, Nail Sakhibullin, Alexander Sklyanov, Roger Smith, Paula Szkody, Zachary P. Vanderbosch
Figure caption: The 0.3–2.3 keV X-ray light curve of SRGeJ0453 during four SRG/eROSITA all-sky surveys. Arrows show 3σ upper limits for X-ray fluxes.
Paper: The Effect of Dust Evolution and Traps on Inner Disk Water Enrichment
Authors: Anusha Kalyaan, Paola Pinilla, Sebastiaan Krijt, Andrea Banzatti, Giovanni Rosotti, Gijs D. Mulders, Michiel Lambrechts, Feng Long, Gregory J. Herczeg
Figure caption: Plots with the results of simulations with planetesimal formation for fiducial initial disk mass M disk = 0.05 M ⊙. The first column shows the time evolution of vapor enrichment for the same simulations performed with planetesimal formation. The second column shows the corresponding total mass of planetesimals formed over time. The third column shows the final planetesimal mass formed at the trap beyond the gap or the snow line (SL) region, for each simulation with the gap at different radial locations. The fourth column shows the final fraction of water ice in the planetesimals that formed at the snow line or the dust trap. The top, middle, and bottom rows, respectively, correspond to v f = 5, 10, and 15 m s−1, inside and outside of the snow line. Line colors are as in Figure 3.
Paper: The Effect of Dust Evolution and Traps on Inner Disk Water Enrichment
Authors: Anusha Kalyaan, Paola Pinilla, Sebastiaan Krijt, Andrea Banzatti, Giovanni Rosotti, Gijs D. Mulders, Michiel Lambrechts, Feng Long, Gregory J. Herczeg
Figure caption: The left panel shows the time evolution of vapor enrichment in the inner disk, i.e., the mass of water vapor within the snow line region at time t, normalized to the mass of water vapor (within the snow line) at time t = 0, for simulations with dust growth and fragmentation. The right panel shows the time evolution of vapor abundance, i.e., the mass of vapor within the snow line region normalized to the mass of gas within the snow line region for the same simulations. Different colors denote profiles for simulations where the gap is located at different radii. The black dashed line shows the case with no gap for comparison. Fiducial v f = 5 m s−1 both inside and outside of the snow line is assumed.
Paper: The Effect of Dust Evolution and Traps on Inner Disk Water Enrichment
Authors: Anusha Kalyaan, Paola Pinilla, Sebastiaan Krijt, Andrea Banzatti, Giovanni Rosotti, Gijs D. Mulders, Michiel Lambrechts, Feng Long, Gregory J. Herczeg
Figure caption: The left panel shows the time evolution of vapor enrichment in the inner disk, i.e., the mass of water vapor within the snow line region at time t, normalized to the mass of water vapor within the snow line at time t = 0, for simulations without dust growth or fragmentation. The right panel shows time evolution of vapor abundance, i.e., mass of vapor within the snow line region normalized to the mass of gas within the snow line region, for the same simulations. Different colors denote profiles for simulations where the gap is located at different radii. The black dashed line shows the case with no gap for comparison.
Paper: The Effect of Dust Evolution and Traps on Inner Disk Water Enrichment
Authors: Anusha Kalyaan, Paola Pinilla, Sebastiaan Krijt, Andrea Banzatti, Giovanni Rosotti, Gijs D. Mulders, Michiel Lambrechts, Feng Long, Gregory J. Herczeg
Figure caption: Time evolution of vapor enrichment for different gap depths at three different radial locations: 7 au (left panel), 30 au (middle panel), and 100 au (right panel). Different colors denote different gap depths (yellow denotes a shallower gap and brown denotes a deeper gap than fiducial). The black dashed line shows the case with no gap for comparison. Fiducial v f = 5 m s−1 both inside and outside of the snow line is assumed.
Paper: The Effect of Dust Evolution and Traps on Inner Disk Water Enrichment
Authors: Anusha Kalyaan, Paola Pinilla, Sebastiaan Krijt, Andrea Banzatti, Giovanni Rosotti, Gijs D. Mulders, Michiel Lambrechts, Feng Long, Gregory J. Herczeg
Figure caption: Time evolution of vapor enrichment for simulations with one gap (left panel), two gaps (middle panel), and three gaps (right panel) with fiducial v f = 5 m s−1 both inside and outside of the snow line, and with planetesimal formation. Colors denote specific gap locations; solid colored lines denote deep gaps at those locations, while dotted–dashed colored lines denote shallow gap(s) at those locations. The dotted line in right panel denotes the case with two shallow interior gaps, along with a deep outer gap. The black dashed line shows the no-gap case for comparison, in each panel.
Paper: The Effect of Dust Evolution and Traps on Inner Disk Water Enrichment
Authors: Anusha Kalyaan, Paola Pinilla, Sebastiaan Krijt, Andrea Banzatti, Giovanni Rosotti, Gijs D. Mulders, Michiel Lambrechts, Feng Long, Gregory J. Herczeg
Figure caption: Grid of simulations performed for a range of fragmentation velocity v f, and turbulent viscosity α. Rows from top to bottom show simulations for α = 1 × 10−4, 5 × 10−4, 1 × 10−3, and 5 × 10−3, respectively. The first three columns from left to right show v f = 1 m s−1, 5 m s−1, and 10 m s−1 (for both inside and outside the snow line). The last column shows the case with v f = 1 m s−1 inside the snow line and 10 m s−1 outside of it. Colors and lines are as in Figure 3. Note that Figure 3(a) is reproduced in the second panel of the third row to show the complete grid.
Paper: The Effect of Dust Evolution and Traps on Inner Disk Water Enrichment
Authors: Anusha Kalyaan, Paola Pinilla, Sebastiaan Krijt, Andrea Banzatti, Giovanni Rosotti, Gijs D. Mulders, Michiel Lambrechts, Feng Long, Gregory J. Herczeg
Figure caption: Time evolution of vapor enrichment for simulations performed with a range of particle and vapor diffusivities. The top row shows simulations varying the particle diffusivity; the bottom row shows simulations varying the vapor diffusivity. Fiducial v f = 5 m s−1 both inside and outside of the snow line is assumed. Colors and lines are as in Figure 3.
Paper: The Effect of Dust Evolution and Traps on Inner Disk Water Enrichment
Authors: Anusha Kalyaan, Paola Pinilla, Sebastiaan Krijt, Andrea Banzatti, Giovanni Rosotti, Gijs D. Mulders, Michiel Lambrechts, Feng Long, Gregory J. Herczeg
Figure caption: Schematic figure presenting our multimillion-year volatile-inclusive disk evolution model with disk structure (top). Icy particles radially drift inwards, enriching the inner disk with water vapor. The vapor mass typically rises with incoming pebble drift, peaks, and then declines with time as disk mass accretes onto the star (bottom).
Paper: The Dependence of the Location and Pressure Variations of the Martian Magnetic Pileup Boundary on the Interplanetary Magnetic Field: An MHD Simulation Study
Authors: M. Wang, K. Xu, J. Y. Lu, M. X. Yin, H. Y. Sui, Z. J. Guan, J. Q. Zhang
Figure caption: Pressure conditions along the Sun–Mars line on the dayside. The strongest Martian crustal magnetic field is located on the dayside (longitude = 180° W, latitude = 0° N) under the Parker IMF (B  X  = −1.6776 nT, B  Y  = 2.4871 nT, and B  Z  = 0 nT). (a) Pressure profiles along the Sun–Mars line on the dayside. The black, blue, and red solid lines represent the solar wind dynamic pressure (P  d  = ρ V 2, where ρ and V are the solar wind density and velocity), the total magnetic pressure (P  B  = B 2/2μ 0, where B is the magnetic field strength and μ 0 is the vacuum permeability), and the solar wind thermal pressure (P th = nkT, where n is the number density of solar wind, k = 1.3807 × 10−23 J K−1 is the Boltzmann constant, and T is the temperature of the plasma). The dashed black line stands for the location where P  B  equals P th (r 0 = 1.274 R  M ), which is regarded as the subsolar standoff point of the MPB. (b) The solar wind pressure coefficient, k, describes the ratio of the total magnetic and thermal pressure to the upstream solar wind dynamic pressure. k is 0.9308 just outside the subsolar standoff point of the MPB. (c) The magnetic compression factor, f, is the ratio of the magnetic field intensity to that of the initial time state of the pure Martian crustal field of the Arkani-Hamed (2001) model at the same location, f = 3.388, just inside the subsolar standoff point of the MPB.
Paper: The Effect of Dust Evolution and Traps on Inner Disk Water Enrichment
Authors: Anusha Kalyaan, Paola Pinilla, Sebastiaan Krijt, Andrea Banzatti, Giovanni Rosotti, Gijs D. Mulders, Michiel Lambrechts, Feng Long, Gregory J. Herczeg
Figure caption: Figures showing the mass of planetesimals formed over time at either the water snow line or dust trap (pressure bump) beyond the gap, when planetesimal formation is included. The left column shows simulations with a fiducial disk mass; the right column shows higher disk masses. The top, middle, and bottom rows represent v frag = 5, 10, and 15 m s−1, respectively. In each case, planetesimal formation takes place for a limited duration, after which the mass of planetesimals formed remains constant with time.
Paper: The Effect of Dust Evolution and Traps on Inner Disk Water Enrichment
Authors: Anusha Kalyaan, Paola Pinilla, Sebastiaan Krijt, Andrea Banzatti, Giovanni Rosotti, Gijs D. Mulders, Michiel Lambrechts, Feng Long, Gregory J. Herczeg
Figure caption: Dust density distributions for the same simulations depicted in Figure 12 at two different snapshots in time: at 0.06 Myr (left column) and at 0.4 Myr (right column). Rows show simulations with a shallower gap (top) or a deeper gap (bottom). The black dashed line shows the maximum particle size ﹩{a}_{\max }﹩(r) as computed by the reconstruction model of Birnstiel et al. (2015); the vertical brown dashed line shows the fragmentation radius, r f, representing the radial extent of the fragmentation-dominated region in disks, also computed by the same model.
Paper: The Effect of Dust Evolution and Traps on Inner Disk Water Enrichment
Authors: Anusha Kalyaan, Paola Pinilla, Sebastiaan Krijt, Andrea Banzatti, Giovanni Rosotti, Gijs D. Mulders, Michiel Lambrechts, Feng Long, Gregory J. Herczeg
Figure caption: Dust surface densities for large (blue lines) and small particles (brown lines) at the snow line (left column) and at traps (right column) for two simulations of different gap depths for a gap at 7 au. The top row shows a simulation with a gap depth of 1.5 × α 0; the bottom row shows a simulation with a gap depth of 10 × α 0.
Paper: The Effect of Dust Evolution and Traps on Inner Disk Water Enrichment
Authors: Anusha Kalyaan, Paola Pinilla, Sebastiaan Krijt, Andrea Banzatti, Giovanni Rosotti, Gijs D. Mulders, Michiel Lambrechts, Feng Long, Gregory J. Herczeg
Figure caption: Plots shown are similar to Figure 7, but with a higher initial disk mass of M disk = 0.1 M ⊙.
Paper: The Effect of Dust Evolution and Traps on Inner Disk Water Enrichment
Authors: Anusha Kalyaan, Paola Pinilla, Sebastiaan Krijt, Andrea Banzatti, Giovanni Rosotti, Gijs D. Mulders, Michiel Lambrechts, Feng Long, Gregory J. Herczeg
Figure caption: Plots showing “vapor abundance,” i.e., the ratio of the mass of vapor within the snow line to the mass of bulk gas within the snow line, for simulations with a radially uniform fragmentation velocity v f = 1 m s−1 (left) and 10 m s−1 (right). Lines and colors are as in Figure 2.
Paper: The Effect of Dust Evolution and Traps on Inner Disk Water Enrichment
Authors: Anusha Kalyaan, Paola Pinilla, Sebastiaan Krijt, Andrea Banzatti, Giovanni Rosotti, Gijs D. Mulders, Michiel Lambrechts, Feng Long, Gregory J. Herczeg
Figure caption: Plots showing the fraction of the total initial pebble mass trapped beyond the gap at each time for simulations with v frag = 1 m s−1 (left), 5 m s−1 (middle), and 10 m s−1 (right).
Paper: The Effect of Dust Evolution and Traps on Inner Disk Water Enrichment
Authors: Anusha Kalyaan, Paola Pinilla, Sebastiaan Krijt, Andrea Banzatti, Giovanni Rosotti, Gijs D. Mulders, Michiel Lambrechts, Feng Long, Gregory J. Herczeg
Figure caption: Plot showing the mass of gas present within the snow line over time for typical simulations with a fiducial initial disk mass. Note that the snow line moves slightly inward with time.
Paper: The Dependence of the Location and Pressure Variations of the Martian Magnetic Pileup Boundary on the Interplanetary Magnetic Field: An MHD Simulation Study
Authors: M. Wang, K. Xu, J. Y. Lu, M. X. Yin, H. Y. Sui, Z. J. Guan, J. Q. Zhang
Figure caption: The dependence of the MPB subsolar standoff distance (r 0 in panel (a)), the solar wind pressure coefficient (k in panel (b)), and the magnetic compression factor (f in panel (c)) on the IMF components of B  X  (black triangles), B  Y  (red squares), and B  Z  (blue circles) when the strongest Martian crustal magnetic field (longitude = 180° W, latitude = 0° N) is located on the dayside. The IMF conditions were set with one component having a nonzero value, while the two other components were null. The IMF components of B  X , B  Y , and B  Z  vary from −5 to 5 nT.