adsabs/AstroCLIMB huggingface dataset:
Paper: ALMA Observations of CO Emission from Luminous Lyman-break Galaxies at z = 6.0293–6.2037
Authors: Yoshiaki Ono, Seiji Fujimoto, Yuichi Harikane, Masami Ouchi, Livia Vallini, Andrea Ferrara, Takatoshi Shibuya, Andrea Pallottini, Akio K. Inoue, Masatoshi Imanishi, Kazuhiro Shimasaku, Takuya Hashimoto, Chien-Hsiu Lee, Yuma Sugahara, Yoichi Tamura, Kotaro Kohno, Malte Schramm
Figure caption: ΣSFR vs. Σgas. The red filled circle is our ALMA result for a luminous LBG at z = 6 with ≃4σ CO(6–5) detection, J0235–0532, in the case of T dust = 50 K and SFRtot = SFRUV + SFRIR,2σ . The error bar along the y-axis considers the case of a higher dust temperature of T dust = 80 K and the minimum SFR case of SFRtot = SFRUV. The red filled triangle and diamond are also our ALMA results for the other luminous LBGs at z = 6, J1211–0118 and J0217–0208, respectively, which show no significant CO(6–5) detection. The red arrows correspond to the 3σ limits. We also present the results for our z = 6 luminous LBGs adopting the CO SLED and α CO for Althaea for their total gas mass estimates, and the previously obtained [C II] sizes as their gas sizes (red open circle: J0235–0532; red open triangle: J1211–0118; red open diamond: J0217–0208; for details, see Section 5.4). The blue squares represent the results of LBG-1 and HZ10 from left to right (Pavesi et al. 2019). Note that the data point of HZ10 is shifted by +0.1 dex along the x-axis for visibility. The blue arrow represents the 3σ limit. The orange squares are the results of AzTEC-3 and CRLE from left to right (Riechers et al. 2010, 2014; Pavesi et al. 2018; see also Pavesi et al. 2019). The brown star denotes the average of the four data points of J0235–0532, HZ10, AzTEC-3, and CRLE as the average KS relation at z = 5–6, although the number of high-z sources whose ΣSFR and Σgas are estimated is limited. The black open triangles and squares denote local spiral galaxies and starbursts compiled by de los Reyes & Kennicutt (2019) and Kennicutt & De Los Reyes (2021), respectively. The blue solid line corresponds to the KS relation, ﹩\mathrm{log}{{\rm{\Sigma }}}_{\mathrm{SFR}}=(1.50\pm 0.02)\mathrm{log}{{\rm{\Sigma }}}_{\mathrm{gas}}-3.87\pm 0.04﹩ (Kennicutt & De Los Reyes 2021) and the blue shaded region represents the ΣSFR values that can be obtained when the two parameters of the KS relation change within the 2σ uncertainties. Note that the ΣSFR values in de los Reyes & Kennicutt (2019) and Kennicutt & De Los Reyes (2021) are corrected by a factor of α KC (Section 1) to consider the IMF difference (Table E1).
Paper: ALMA Observations of CO Emission from Luminous Lyman-break Galaxies at z = 6.0293–6.2037
Authors: Yoshiaki Ono, Seiji Fujimoto, Yuichi Harikane, Masami Ouchi, Livia Vallini, Andrea Ferrara, Takatoshi Shibuya, Andrea Pallottini, Akio K. Inoue, Masatoshi Imanishi, Kazuhiro Shimasaku, Takuya Hashimoto, Chien-Hsiu Lee, Yuma Sugahara, Yoichi Tamura, Kotaro Kohno, Malte Schramm
Figure caption: Top left: L CO(6−5)/L [C II] vs. L [C II]/L IR. The red circle is our ALMA result for a luminous LBG at z = 6 with ≃4σ CO(6–5) detection, J0235–0532, in the case of T dust = 50 K, and the lower error bar along the x-axis considers the higher dust temperature case of T dust = 80 K. The red triangle and diamond are also our ALMA results for the other luminous LBGs at z = 6, J1211–0118 and J0217–0208, respectively, which show no significant CO(6–5) detection. The red arrows correspond to the 3σ limits. The solid and dashed curves represent the theoretical calculations with the PDRT with constant densities of hydrogen nuclei, n H, in units of cm−3, and FUV (6–13.6 eV) radiation fields, U UV, in units of the average interstellar radiation field in the vicinity of the Sun, G 0 = 1.6 × 10−3 erg s−1 cm−2 (Habing 1968), respectively. The blue arrow in the upper right corner represents the amount of shift when ﹩{f}_{[{\rm{C}}\,{\rm\small{II}}]}^{(\mathrm{ion})}﹩ increases by 0.1. The green arrow in the upper right corner shows the systematic uncertainties of the CMB effect on the [C II] emission (Kohandel et al. 2019). Top right: L CO(1−0)/L [C II] vs. L [C II]/L IR. The orange squares denote LIRGs and ULIRGs (Rosenberg et al. 2015). The blue downward triangles and cyan triangles represent local SFGs and Galactic star-forming regions, respectively (Stacey et al. 1991). The magenta diamonds represent high-z quasars (Benford et al. 1999; Maiolino et al. 2005; Iono et al. 2006; Wagg et al. 2012, 2014; Leipski et al. 2013; Stefan et al. 2015; Wang et al. 2016; Venemans et al. 2017b; compiled by Shao et al. 2019). The solid and dashed curves are the same as in the left panel. In both panels, the CO line luminosities are multiplied by a factor of two as recommended by Kaufman et al. (1999) (for details, see the text in Section 5.1; see also Shao et al. 2019). Bottom: same as the top left panel, but with the colored shaded regions that roughly correspond to the low-z CO(1–0) results presented in the top right panel.
Paper: ALMA Observations of CO Emission from Luminous Lyman-break Galaxies at z = 6.0293–6.2037
Authors: Yoshiaki Ono, Seiji Fujimoto, Yuichi Harikane, Masami Ouchi, Livia Vallini, Andrea Ferrara, Takatoshi Shibuya, Andrea Pallottini, Akio K. Inoue, Masatoshi Imanishi, Kazuhiro Shimasaku, Takuya Hashimoto, Chien-Hsiu Lee, Yuma Sugahara, Yoichi Tamura, Kotaro Kohno, Malte Schramm
Figure caption: SFR vs. M gas. The red circle is our ALMA result for a luminous LBG at z = 6 with ≃4σ CO(6–5) detection, J0235–0532, in the case of T dust = 50 K and SFRtot = SFRUV + SFRIR,2σ . The error bar along the y-axis considers the case of a higher dust temperature of T dust = 80 K and the minimum SFR case of SFRtot = SFRUV. Note that, although the intrinsic CO flux and thus the M gas value become somewhat larger with a higher dust temperature, such a systematic uncertainty is much smaller than the uncertainty in the CO flux measurement. The red triangle and diamond are also our ALMA results for the other luminous LBGs at z = 6, J1211–0118 and J0217–0208, respectively, which show no significant CO(6–5) detection. The red arrows correspond to the 3σ limits. The blue squares represent the results of LBG-1 and HZ10 from left to right (Pavesi et al. 2019). The blue arrow represents the 3σ limit. The orange squares are the results of AzTEC-3 and CRLE from left to right (Riechers et al. 2010, 2014; Pavesi et al. 2018; see also Pavesi et al. 2019). The black filled downward triangles are the results of SFGs with M star > 3 × 1010 M ⊙ at z ∼ 0–4 using stacked dust SEDs (Béthermin et al. 2015). The black open downward triangles show the results of SFGs with M star > 2 × 1010 M ⊙ at z ∼ 1–6 based on submillimeter dust continuum measurements (Scoville et al. 2016). The black open triangles are the results for low-z galaxies at z = 0.01–0.05 (Saintonge et al. 2017).
Paper: ALMA Observations of CO Emission from Luminous Lyman-break Galaxies at z = 6.0293–6.2037
Authors: Yoshiaki Ono, Seiji Fujimoto, Yuichi Harikane, Masami Ouchi, Livia Vallini, Andrea Ferrara, Takatoshi Shibuya, Andrea Pallottini, Akio K. Inoue, Masatoshi Imanishi, Kazuhiro Shimasaku, Takuya Hashimoto, Chien-Hsiu Lee, Yuma Sugahara, Yoichi Tamura, Kotaro Kohno, Malte Schramm
Figure caption: Redshift evolution of the gas depletion time, t dep = M gas/SFR. The red circle is our ALMA result for a luminous LBG at z = 6 with ≃4σ CO(6–5) detection, J0235–0532, in the case of T dust = 50 K and SFRtot = SFRUV + SFRIR,2σ . The error bar along the y-axis for J0235–0532 considers the case of a higher dust temperature of T dust = 80 K and the minimum SFR case of SFRtot = SFRUV. The red triangle and diamond are also our ALMA results for the other luminous LBGs at z = 6, J1211–0118 and J0217–0208, respectively, which show no significant CO(6–5) detection. The red arrows correspond to the 3σ limits. The blue squares represent the results of LBG-1 and HZ10 from left to right (Pavesi et al. 2019). The blue arrow represents the 3σ limit. The orange squares are the results of AzTEC-3 and CRLE from left to right (Riechers et al. 2010, 2014; Pavesi et al. 2018; see also Pavesi et al. 2019). The blue filled triangles show the average results of z = 4.4–5.9 LBGs with M star = 108.4−11 M ⊙ obtained in the ALPINE survey (Dessauges-Zavadsky et al. 2020), where M gas are estimated from the [C II] luminosities. The black filled triangles denote the results based on CO observations of z ∼ 3 LBGs (Magdis et al. 2017). The black filled downward triangles are the results of SFGs with M star > 3 × 1010 M ⊙ using stacked dust SEDs (Béthermin et al. 2015). The black open downward triangles show the results of SFGs with M star > 2 × 1010 M ⊙ based on submillimeter dust continuum measurements (Schinnerer et al. 2016; Scoville et al. 2016). The black open squares are the results for lensed/unlensed dusty starburst sources compiled by Aravena et al. (2016). The dashed and dotted lines correspond to the curves of t dep ∝ (1 + z)−1.0 and t dep ∝ (1 + z)−1.5 (e.g., Davé et al. 2012; Tacconi et al. 2013), which are normalized to the typical gas depletion time of 1.5 Gyr observed for local galaxies (Leroy et al. 2008; Bigiel et al. 2011; Saintonge et al. 2011, 2012; see also Saintonge et al. 2013).
Paper: Turbulent Reacceleration of Streaming Cosmic Rays
Authors: Chad Bustard, S. Peng Oh
Figure caption: Left: growth times as a function of plasma β for CRs with (dashed lines) and without (solid lines) streaming, both with parallel diffusion coefficients of κ ∣∣ = 0.15c  s  L 0 such that the growth time is near the minimum. Different colors correspond to different grid sizes. With only diffusion, growth times are near the minimum value (see Figure 1), but streaming losses significantly offset the energy gain when β is low. Right: ratio of growth times with and without streaming. The dashed blue line shows the analytic estimate for the κ < v ph L 0 regime (Equation (12)), and the blue dotted–dashed line shows the analytic estimate for the κ > > v ph L 0 regime (Equation (13)). Compared to canonical rates assuming pure diffusion, reacceleration is less efficient in low-β environments when streaming is included.
Paper: ALMA Observations of CO Emission from Luminous Lyman-break Galaxies at z = 6.0293–6.2037
Authors: Yoshiaki Ono, Seiji Fujimoto, Yuichi Harikane, Masami Ouchi, Livia Vallini, Andrea Ferrara, Takatoshi Shibuya, Andrea Pallottini, Akio K. Inoue, Masatoshi Imanishi, Kazuhiro Shimasaku, Takuya Hashimoto, Chien-Hsiu Lee, Yuma Sugahara, Yoichi Tamura, Kotaro Kohno, Malte Schramm
Figure caption: Gas fraction, f gas = M gas/(M gas + M star), as a function of SFR. The red circle is our ALMA result for a luminous LBG at z = 6 with ≃4σ CO(6–5) detection, J0235–0532, in the case of T dust = 50 K and SFRtot = SFRUV + SFRIR,2σ . The error bar along the y-axis considers the case of a higher dust temperature of T dust = 80 K and the minimum SFR case of SFRtot = SFRUV. The red triangle and diamond are also our ALMA results for the other luminous LBGs at z = 6, J1211–0118 and J0217–0208, respectively, which show no significant CO(6–5) detection. The red arrows correspond to the 3σ limits. The blue squares represent the results of LBG-1 and HZ10 from left to right (Pavesi et al. 2019). The blue arrow represents the 3σ limit. The orange squares are the results of AzTEC-3 and CRLE from left to right (Riechers et al. 2010, 2014; Pavesi et al. 2018; see also Pavesi et al. 2019). The black filled downward triangles are the results of SFGs with M star > 3 × 1010 M ⊙ at z ∼ 0–4 using stacked dust SEDs (Béthermin et al. 2015). The black open downward triangles show the results of SFGs with M star > 2 × 1010 M ⊙ at z ∼ 1–6 based on submillimeter dust continuum measurements (Scoville et al. 2016). The black open triangles are the results for low-z galaxies at z = 0.01–0.05 (Saintonge et al. 2017).
Paper: Turbulent Reacceleration of Streaming Cosmic Rays
Authors: Chad Bustard, S. Peng Oh
Figure caption: CR energy growth times, normalized by the outer scale eddy turnover time (τ eddy) for simulations each with β = 1 but varying ﹩{ \mathcal M }﹩ (different colors). Simulations were run using either v  m /c  s  = 50 (dots) or v  m /c  s  = 100 (x’s); see the Appendix for a full comparison of different v  m  and different resolutions. Lines show analytic expectations assuming isotropic diffusion (solid lines; Ptuskin 1988) and including a correction for anisotropic diffusion (dashed line; Chandran & Maron 2004) for κ > v ph L 0. Simulations match expectations remarkably well for κ < v ph L 0 if one sets L 0/L 1 = 20, i.e., if L 1 represents one cell width. Simulations also reflect the expected decrease in growth time due to anisotropic diffusion.
Paper: ALMA Observations of CO Emission from Luminous Lyman-break Galaxies at z = 6.0293–6.2037
Authors: Yoshiaki Ono, Seiji Fujimoto, Yuichi Harikane, Masami Ouchi, Livia Vallini, Andrea Ferrara, Takatoshi Shibuya, Andrea Pallottini, Akio K. Inoue, Masatoshi Imanishi, Kazuhiro Shimasaku, Takuya Hashimoto, Chien-Hsiu Lee, Yuma Sugahara, Yoichi Tamura, Kotaro Kohno, Malte Schramm
Figure caption: Dust continuum emission maps for our z = 6 luminous LBGs, J1211–0118, J0235–0532, and J0217–0208 from left to right. The red contours are continuum emission at λ rest ≃ 430 μm drawn at 1σ intervals from 1.5σ. Although the dust continuum of J0235 and J0217 may show a ∼2σ signal, in this paper we conservatively use their 3σ upper limits. The blue lines represent negative contours from −1.5σ at 1σ intervals. The red ellipses at the lower left corner denote the ALMA synthesized beams. The gray backgrounds are the Subaru HSC z-band images that capture the rest UV continuum emission from our targets. The size of each image is 10″ × 10″.
Paper: X-Ray Spectroscopic Evidence of Charge Exchange Emission in the Disk of M51
Authors: Shuinai Zhang, 水乃 张, Q. Daniel Wang, Wei Sun, Min Long, Jia Sun, 佳 孙, Li Ji
Figure caption: (a) Chandra/ACIS-S intensity image of M51 in the 0.5–1.2 keV band. The green rectangles (﹩8^{\prime} \times 4\buildrel{\,\prime}\over{.} 4﹩) represent the dispersion directions, as well as the widths of the regions covered by the RGS observations, while their on-axis positions are marked as the green pluses (“+”). The actual spectral extraction regions for the NHS are outlined by the four cyan dashed rectangles with the widths of 1′ or 1.′6 in the cross-dispersion direction. (b) The same Chandra count intensity image of M51, but with detected discrete sources removed. The yellow elliptical region is defined as the NHS region, while the cyan annular region with the elliptical region excluded is defined as the disk region without NHS. The image is overlaid with white curves sketching out prominent neutral atomic gas features (mainly spiral arms) as seen in panel (c), where the field is seen in the H I 21 cm line emission in units of Jy beam−1·m s−1. While the sketch is in pale violet red in panel (c), a vertical arm segment “A” is highlighted with the red color. The cross symbols (“×”) in all the three panels mark the galactic center and the reference point for the spectral extraction.
Paper: X-Ray Spectroscopic Evidence of Charge Exchange Emission in the Disk of M51
Authors: Shuinai Zhang, 水乃 张, Q. Daniel Wang, Wei Sun, Min Long, Jia Sun, 佳 孙, Li Ji
Figure caption: RGS1 and RGS2 spectra of the NHS (colored coded in blue and green, respectively) in comparison with fitted models: (a) single-temperature APEC thermal plasma (red line) for the diffuse X-ray emission; (b) APEC+ACX; (c) vltnd+ACX (Table 2). In these panels, while the red histogram represents the total model spectra, the black dashed, orange dotted, and magenta dotted–dashed curves represent the point source, thermal plasma, and CX contributions, respectively.
Paper: X-Ray Spectroscopic Evidence of Charge Exchange Emission in the Disk of M51
Authors: Shuinai Zhang, 水乃 张, Q. Daniel Wang, Wei Sun, Min Long, Jia Sun, 佳 孙, Li Ji
Figure caption: Oxygen line intensity maps (left panels, in units of ﹩\mathrm{photon}\,{{\rm{s}}}^{-1}\,{\mathrm{arcsec}}^{-2}﹩) and their corresponding RGS exposure maps (right panels, in units of seconds) of M51. The morphology of the line intensity distribution in the galaxy’s core is distorted because of its location at edges of the RGS field of view. The smaller red boxes (﹩1^{\prime} \times 1^{\prime} ﹩) mark the regions that may be contaminated by the O VIIKβ or O VII i line emission from the galactic core. These contaminated regions, together with noisy regions due to obvious chip gaps, are further masked with the large orange rectangles. The rest are the same as in Figure 1.
Paper: X-Ray Spectroscopic Evidence of Charge Exchange Emission in the Disk of M51
Authors: Shuinai Zhang, 水乃 张, Q. Daniel Wang, Wei Sun, Min Long, Jia Sun, 佳 孙, Li Ji
Figure caption: Illustration of the O VIII map construction for the RGS observation (ID: 0824450901): (a) the count intensity map (without the continuum removal), smoothed with a Gaussian of size comparable to the resolution of the data; (b) the continuum intensity map interpolated from two off-line bands marked by the two shaded regions; (c) the line flux map after the continuum subtraction.
Paper: X-Ray Spectroscopic Evidence of Charge Exchange Emission in the Disk of M51
Authors: Shuinai Zhang, 水乃 张, Q. Daniel Wang, Wei Sun, Min Long, Jia Sun, 佳 孙, Li Ji
Figure caption: ACIS-S spectra of the NHS and the galactic disk of M51 (upper and lower panels) in comparison with the best-fit thermal plasma plus CX models.
Paper: X-Ray Spectroscopic Evidence of Charge Exchange Emission in the Disk of M51
Authors: Shuinai Zhang, 水乃 张, Q. Daniel Wang, Wei Sun, Min Long, Jia Sun, 佳 孙, Li Ji
Figure caption: S/N ratio maps of the O VIII Lyα and the O VII Heα f. The bin size is 25″, similar to that of the RGS resolution.
Paper: Explaining the Moderate UV/X-Ray Correlation in AGN
Authors: Christos Panagiotou, Erin Kara, Michal Dovčiak
Figure caption: Normalized histogram of the maximum CCF between the UVW2 and B light curve, R W2B, in the case of a variable height.
Paper: The Spectral Evolution Patterns and Implications of Gamma-Ray Burst X-Ray Flares
Authors: Lian-Zhong Lü, En-Wei Liang, Bertrand Cordier
Figure caption: Type I: the spectral evolutions of flares are hard-to-soft. The XRT light curves (upper panel of each plot) and spectral indices (lower panel of each plot) as a function of time. The red solid curve in the upper panels is the best fit to the XRT data with a (multiply) broken power law, plus a number of FRED functions. The two vertical straight dotted lines indicate the start and the end time of the flare, respectively. The blue straight line in the lower panels is the linear fit to the spectral indices of the flare.
Paper: The Spectral Evolution Patterns and Implications of Gamma-Ray Burst X-Ray Flares
Authors: Lian-Zhong Lü, En-Wei Liang, Bertrand Cordier
Figure caption:                         Type II: the spectral evolutions of flares are soft-to-hard-to-soft (intensity tracking). Symbols are as in Figure 1.
Paper: (When) Can Wave Heating Balance Optically Thin Radiative Losses in the Corona?
Authors: I. De Moortel, T. A. Howson
Figure caption: Time-distance plot of the density (left panels) and temperature (right panels) at the apex of the loop (z  =  100 Mm and y  =  0 Mm). The top two rows correspond to the lower-density simulations. The top panels have a tuned driver and the middle panels have a detuned driver. The bottom panels correspond to a tuned driver with the higher density. Note that to have comparable color tables, the density for the high-density simulation has been divided by 15.
Paper: (When) Can Wave Heating Balance Optically Thin Radiative Losses in the Corona?
Authors: I. De Moortel, T. A. Howson
Figure caption: Horizontal cross sections at the loop apex (z  =  100 Mm) at t = 1043 s of temperature (top row), density (2nd row), and vorticity (bottom row) for the low-density, tuned simulation (left panels) the high-density, tuned simulation (middle panels), and the low-density, detuned simulation (right panels). Note that to have comparable color tables, the density cross sections for the low-density simulations have been multiplied by three. The vorticity for the tuned simulations has been divided by 10−2 and by 10−7 for the detuned simulation (bottom right).
Paper: (When) Can Wave Heating Balance Optically Thin Radiative Losses in the Corona?
Authors: I. De Moortel, T. A. Howson
Figure caption: Evolution of the maximum (solid lines) and mean (dashed lines) temperatures in the 3D simulation volume. The thick black lines correspond to the low-density, tuned simulation, the thin black lines to the high-density, tuned simulation, and the red lines represent the low-density, detuned simulation. Optically thin radiation is included in all three cases.
Paper: (When) Can Wave Heating Balance Optically Thin Radiative Losses in the Corona?
Authors: I. De Moortel, T. A. Howson
Figure caption: Time-distance plots of the density (nondimensional units) at the apex of the loop (z  =  100 Mm and x  =  0 Mm). The top panel shows the evolution of the density for the detuned simulation whereas the bottom panel corresponds to the tuned driver. For both simulations, the densities correspond to the higher-density setup (i.e., where ρ  e  = 1.67 × 10−12 kg m−3).
Paper: Searching for Propionamide (C2H5CONH2) toward Sagittarius B2 at Centimeter Wavelengths
Authors: Caden Schuessler, Anthony Remijan, Ci Xue, Joshua Carder, Haley Scolati, Brett McGuire
Figure caption: Graphical representation of possible molecular structures by subsequent methyl (CH3) and/or amine (NH2) addition starting with water (H2O). Caveat concerning possible formation routes is the same as in Figure 4.
Paper: (When) Can Wave Heating Balance Optically Thin Radiative Losses in the Corona?
Authors: I. De Moortel, T. A. Howson
Figure caption: The transverse velocity in the midpoint of the domain (x = y = 0 Mm, z = 100 Mm) as a function of time. The black lines correspond to the tuned driver whereas the red lines represent the detuned driver. For comparison, the dotted lines show the corresponding transverse velocity of the driver on the lower boundary (x = y = z = 0 Mm). For both simulations, the densities correspond to the higher-density setup.
Paper: (When) Can Wave Heating Balance Optically Thin Radiative Losses in the Corona?
Authors: I. De Moortel, T. A. Howson
Figure caption: A horizontal cross section of the initial density (i.e., at t  =  0 s).
Paper: (When) Can Wave Heating Balance Optically Thin Radiative Losses in the Corona?
Authors: I. De Moortel, T. A. Howson
Figure caption: A vertical cross section of the initial density (i.e., at t  =  0 s).
Paper: Detailed Calculations of the Efficiency of Planetesimal Accretion in the Core-accretion Model. II. The Effect of Saturn
Authors: Nader Haghighipour, Morris Podolak, Esther Podolak
Figure caption: Interaction of a 100 km rocky planetesimal with the envelope. The top panel shows the planetesimal’s actual path. The dark oval shows the outer edge of the envelope. The position and motion of the planetesimals prior to encountering the envelope is shown by the red arrow. Red points indicate inward motion toward the core, and blue points indicate outward motion away from the core. As shown here, the planetesimal enters and leaves the envelope several times until it is fully captured. The bottom panel shows the amount of the mass that the planetesimal loses during each passage through the envelope.
Paper: Detailed Calculations of the Efficiency of Planetesimal Accretion in the Core-accretion Model. II. The Effect of Saturn
Authors: Nader Haghighipour, Morris Podolak, Esther Podolak
Figure caption: Graphs of the mass deposition of two 1 km rocky planetesimals in terms of distance from the center of Jupiter. Note that the left vertical axis shows the envelope’s temperature and the right vertical axis shows the planetesimal’s relative mass. The black line represents the temperature of the envelope at 1.66 Myr. The red curve shows a planetesimal that penetrates through the envelope and is fully absorbed. The green lines show a planetesimal that undergoes multiple encounters until it is fully accreted. Note that in both cases, full accretion occurs at ∼3000 K.