Caleb K. Harada, Courtney D. Dressing, Stephen R. Kane, Sarah Blunt, Jamie Dietrich, Natalie R. Hinkel, Zhexing Li, Eric Mamajek, Malena Rice, Noah W. Tuchow, Emma V. Turtelboom, Robert A. Wittenmyer
Future large, space-based observatories with starlight suppression technology, e.g., the Habitable Worlds Observatory (HWO), will directly image and characterize nearby Earth-like exoplanets. Prior limits on planet masses and system architectures from radial velocity (RV) measurements of potential exo-Earth hosts are critical to the success of HWO's science goals. Here, we present a uniform analysis of archival RVs from HIRES/Keck and HARPS/ESO of the most promising targets for the HWO exo-Earth survey. We analyze RVs and stellar activity indicators of 90 stars in the NASA ExEP Mission Star List and SPORES-HWO Catalog, finding 33 Keplerian signals associated with known planets and 12 signals associated with stellar activity. We also identify 5 new RV signals that we classify as either planet candidates or sources requiring confirmation, noting that the RV observations are biased toward cooler and less active stars. Assessing the sensitivity of the HIRES and HARPS data, we calculate RV limits ranging from $K_{rm RV} = 0.6 ,{rm m,s}^{-1}$ (HD 10700) to $371 ,{rm m,s}^{-1}$ (HD 17925) in the middle of the conservative habitable zone (HZ), corresponding to projected planet masses of $5.4 ,{rm M_oplus}$ and $10.6 ,{rm M_{Jup}}$ for those stars. The median HZ sensitivity limit of our sample is $M_{rm p} sin i simeq 66 ,{rm M_oplus}$. This work demonstrates the need for future extreme precision radial velocity (EPRV) monitoring of high-priority targets for the next generation of DI missions that will search for habitable extrasolar systems. We advocate for the use of these results in developing future EPRV strategies.
{"title":"SPORES-HWO. II. Limits on Planetary Companions of Future High-contrast Imaging Targets from $>$20 Years of HIRES and HARPS Radial Velocities","authors":"Caleb K. Harada, Courtney D. Dressing, Stephen R. Kane, Sarah Blunt, Jamie Dietrich, Natalie R. Hinkel, Zhexing Li, Eric Mamajek, Malena Rice, Noah W. Tuchow, Emma V. Turtelboom, Robert A. Wittenmyer","doi":"arxiv-2409.10679","DOIUrl":"https://doi.org/arxiv-2409.10679","url":null,"abstract":"Future large, space-based observatories with starlight suppression\u0000technology, e.g., the Habitable Worlds Observatory (HWO), will directly image\u0000and characterize nearby Earth-like exoplanets. Prior limits on planet masses\u0000and system architectures from radial velocity (RV) measurements of potential\u0000exo-Earth hosts are critical to the success of HWO's science goals. Here, we\u0000present a uniform analysis of archival RVs from HIRES/Keck and HARPS/ESO of the\u0000most promising targets for the HWO exo-Earth survey. We analyze RVs and stellar\u0000activity indicators of 90 stars in the NASA ExEP Mission Star List and\u0000SPORES-HWO Catalog, finding 33 Keplerian signals associated with known planets\u0000and 12 signals associated with stellar activity. We also identify 5 new RV\u0000signals that we classify as either planet candidates or sources requiring\u0000confirmation, noting that the RV observations are biased toward cooler and less\u0000active stars. Assessing the sensitivity of the HIRES and HARPS data, we\u0000calculate RV limits ranging from $K_{rm RV} = 0.6 ,{rm m,s}^{-1}$ (HD\u000010700) to $371 ,{rm m,s}^{-1}$ (HD 17925) in the middle of the conservative\u0000habitable zone (HZ), corresponding to projected planet masses of $5.4 ,{rm\u0000M_oplus}$ and $10.6 ,{rm M_{Jup}}$ for those stars. The median HZ\u0000sensitivity limit of our sample is $M_{rm p} sin i simeq 66 ,{rm\u0000M_oplus}$. This work demonstrates the need for future extreme precision radial\u0000velocity (EPRV) monitoring of high-priority targets for the next generation of\u0000DI missions that will search for habitable extrasolar systems. We advocate for\u0000the use of these results in developing future EPRV strategies.","PeriodicalId":501209,"journal":{"name":"arXiv - PHYS - Earth and Planetary Astrophysics","volume":"94 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142263742","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Sahl Rowther, Daniel J. Price, Christophe Pinte, Rebecca Nealon, Farzana Meru, Richard Alexander
Irradiation from the central star controls the temperature structure in protoplanetary discs. Yet simulations of gravitational instability typically use models of stellar irradiation with varying complexity, or ignore it altogether, assuming heat generated by spiral shocks is balanced by cooling, leading to a self-regulated state. In this paper, we perform simulations of irradiated, gravitationally unstable protoplanetary discs using 3D hydrodynamics coupled with live Monte-Carlo radiative transfer. We find that the resulting temperature profile is approximately constant in time, since the thermal effects of the star dominate. Hence, the disc cannot regulate gravitational instabilities by adjusting the temperatures in the disc. In a 0.1 Solar mass disc, the disc instead adjusts by angular momentum transport induced by the spiral arms, leading to steadily decreasing surface density, and hence quenching of the instability. Thus, strong spiral arms caused by self-gravity would not persist for longer than ten thousand years in the absence of fresh infall, although weak spiral structures remain present over longer timescales. Using synthetic images at 1.3mm, we find that spirals formed in irradiated discs are challenging to detect. In higher mass discs, we find that fragmentation is likely because the dominant stellar irradiation overwhelms the stabilising influence of PdV work and shock heating in the spiral arms.
{"title":"Short-Lived Gravitational Instability in Isolated Irradiated Discs","authors":"Sahl Rowther, Daniel J. Price, Christophe Pinte, Rebecca Nealon, Farzana Meru, Richard Alexander","doi":"arxiv-2409.10765","DOIUrl":"https://doi.org/arxiv-2409.10765","url":null,"abstract":"Irradiation from the central star controls the temperature structure in\u0000protoplanetary discs. Yet simulations of gravitational instability typically\u0000use models of stellar irradiation with varying complexity, or ignore it\u0000altogether, assuming heat generated by spiral shocks is balanced by cooling,\u0000leading to a self-regulated state. In this paper, we perform simulations of\u0000irradiated, gravitationally unstable protoplanetary discs using 3D\u0000hydrodynamics coupled with live Monte-Carlo radiative transfer. We find that\u0000the resulting temperature profile is approximately constant in time, since the\u0000thermal effects of the star dominate. Hence, the disc cannot regulate\u0000gravitational instabilities by adjusting the temperatures in the disc. In a 0.1\u0000Solar mass disc, the disc instead adjusts by angular momentum transport induced\u0000by the spiral arms, leading to steadily decreasing surface density, and hence\u0000quenching of the instability. Thus, strong spiral arms caused by self-gravity\u0000would not persist for longer than ten thousand years in the absence of fresh\u0000infall, although weak spiral structures remain present over longer timescales.\u0000Using synthetic images at 1.3mm, we find that spirals formed in irradiated\u0000discs are challenging to detect. In higher mass discs, we find that\u0000fragmentation is likely because the dominant stellar irradiation overwhelms the\u0000stabilising influence of PdV work and shock heating in the spiral arms.","PeriodicalId":501209,"journal":{"name":"arXiv - PHYS - Earth and Planetary Astrophysics","volume":"16 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142263741","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
A. Castro-González, V. Bourrier, J. Lillo-Box, J. -B. Delisle, D. J. Armstrong, D. Barrado, A. C. M. Correia
Atmospheric and dynamical processes are thought to play a major role in shaping the distribution of close-in exoplanets. A striking feature of such distribution is the Neptunian desert, a dearth of Neptunes on the shortest-period orbits. We aimed to define the boundaries of the Neptunian desert and study its transition into the savanna, a moderately populated region at larger orbital distances. We built a sample of planets and candidates based on the Kepler DR25 catalogue and weighed it according to the transit and detection probabilities. We delimited the Neptunian desert as the close-in region of the period-radius space with no planets at a 3$sigma$ level, and provide the community with simple, ready-to-use approximate boundaries. We identified an overdensity of planets separating the Neptunian desert from the savanna (3.2 days $ lessapprox P_{rm orb}$ $lessapprox$ 5.7 days) that stands out at a 4.7$sigma$ level above the desert and at a 3.5$sigma$ level above the savanna, which we propose to call the Neptunian ridge. The period range of the ridge matches that of the hot Jupiter pileup ($simeq$3-5 days), which suggests that similar evolutionary processes might act on both populations. We find that the occurrence fraction between the pileup and warm Jupiters is about twice that between the Neptunian ridge and savanna. Our revised landscape supports a previous hypothesis that a fraction of Neptunes were brought to the edge of the desert (i.e. the newly identified ridge) through high-eccentricity tidal migration (HEM) late in their life, surviving the evaporation that eroded Neptunes having arrived earlier in the desert. The ridge thus appears as a true physical feature illustrating the interplay between photoevaporation and HEM, providing further evidence of their role in shaping the distribution of close-in Neptunes.
{"title":"Mapping the exo-Neptunian landscape. A ridge between the desert and savanna","authors":"A. Castro-González, V. Bourrier, J. Lillo-Box, J. -B. Delisle, D. J. Armstrong, D. Barrado, A. C. M. Correia","doi":"arxiv-2409.10517","DOIUrl":"https://doi.org/arxiv-2409.10517","url":null,"abstract":"Atmospheric and dynamical processes are thought to play a major role in\u0000shaping the distribution of close-in exoplanets. A striking feature of such\u0000distribution is the Neptunian desert, a dearth of Neptunes on the\u0000shortest-period orbits. We aimed to define the boundaries of the Neptunian\u0000desert and study its transition into the savanna, a moderately populated region\u0000at larger orbital distances. We built a sample of planets and candidates based\u0000on the Kepler DR25 catalogue and weighed it according to the transit and\u0000detection probabilities. We delimited the Neptunian desert as the close-in\u0000region of the period-radius space with no planets at a 3$sigma$ level, and\u0000provide the community with simple, ready-to-use approximate boundaries. We\u0000identified an overdensity of planets separating the Neptunian desert from the\u0000savanna (3.2 days $ lessapprox P_{rm orb}$ $lessapprox$ 5.7 days) that\u0000stands out at a 4.7$sigma$ level above the desert and at a 3.5$sigma$ level\u0000above the savanna, which we propose to call the Neptunian ridge. The period\u0000range of the ridge matches that of the hot Jupiter pileup ($simeq$3-5 days),\u0000which suggests that similar evolutionary processes might act on both\u0000populations. We find that the occurrence fraction between the pileup and warm\u0000Jupiters is about twice that between the Neptunian ridge and savanna. Our\u0000revised landscape supports a previous hypothesis that a fraction of Neptunes\u0000were brought to the edge of the desert (i.e. the newly identified ridge)\u0000through high-eccentricity tidal migration (HEM) late in their life, surviving\u0000the evaporation that eroded Neptunes having arrived earlier in the desert. The\u0000ridge thus appears as a true physical feature illustrating the interplay\u0000between photoevaporation and HEM, providing further evidence of their role in\u0000shaping the distribution of close-in Neptunes.","PeriodicalId":501209,"journal":{"name":"arXiv - PHYS - Earth and Planetary Astrophysics","volume":"34 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142263745","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
The formation of planetary systems has historically been considered in isolation, decoupled from processes on galactic scales. Recent findings employing data from ESA's Gaia mission challenge this narrative, identifying trends in planet occurrence with galactic kinematics and stellar age. The findings indicate changes in planet occurrence over and above the predicted changes from metallicity variation within the Milky Way, so that changes to stellar metallicity alone (long understood to be deterministic in planet outcomes) cannot explain the trends entirely. The scope of potential factors influencing planet formation has grown progressively wider, with accompanying theoretical support for galactic-scale influences upon planet formation. In this manuscript, we investigate specifically how changes to the rate of Systems of Tightly-packed Inner Planets (STIPs) could manifest as a trend in planet occurrence with galactic height. We focus our study upon M dwarf planetary systems for two reasons: first, they host STIPs at high rates, and secondly, their longevity makes them useful probes for kinematic trends over Gyr. We consider two models for a varying STIP rate: one in which STIP likelihood is determined by stellar age alone, irrespective of galactic time, and another in which the STIP likelihood suddenly increased in recent galactic history. Both models, which impose a higher STIP likelihood among younger stars, produce a negative gradient in planet occurrence with increasing height from the galactic midplane. We find that a step function model in which STIP likelihood increased by a factor of several ~a few Gyr ago resembles an observed trend among FGK dwarfs. We consider plausible physical mechanisms that could mimic the hypothesized model, given known links between STIP occurrence and other stellar and planetary properties.
{"title":"Tuning the Rate of Tightly Packed Systems To Produce Planet Occurrence Trends with Galactic Height","authors":"Sarah Ballard","doi":"arxiv-2409.10485","DOIUrl":"https://doi.org/arxiv-2409.10485","url":null,"abstract":"The formation of planetary systems has historically been considered in\u0000isolation, decoupled from processes on galactic scales. Recent findings\u0000employing data from ESA's Gaia mission challenge this narrative, identifying\u0000trends in planet occurrence with galactic kinematics and stellar age. The\u0000findings indicate changes in planet occurrence over and above the predicted\u0000changes from metallicity variation within the Milky Way, so that changes to\u0000stellar metallicity alone (long understood to be deterministic in planet\u0000outcomes) cannot explain the trends entirely. The scope of potential factors\u0000influencing planet formation has grown progressively wider, with accompanying\u0000theoretical support for galactic-scale influences upon planet formation. In\u0000this manuscript, we investigate specifically how changes to the rate of Systems\u0000of Tightly-packed Inner Planets (STIPs) could manifest as a trend in planet\u0000occurrence with galactic height. We focus our study upon M dwarf planetary\u0000systems for two reasons: first, they host STIPs at high rates, and secondly,\u0000their longevity makes them useful probes for kinematic trends over Gyr. We\u0000consider two models for a varying STIP rate: one in which STIP likelihood is\u0000determined by stellar age alone, irrespective of galactic time, and another in\u0000which the STIP likelihood suddenly increased in recent galactic history. Both\u0000models, which impose a higher STIP likelihood among younger stars, produce a\u0000negative gradient in planet occurrence with increasing height from the galactic\u0000midplane. We find that a step function model in which STIP likelihood increased\u0000by a factor of several ~a few Gyr ago resembles an observed trend among FGK\u0000dwarfs. We consider plausible physical mechanisms that could mimic the\u0000hypothesized model, given known links between STIP occurrence and other stellar\u0000and planetary properties.","PeriodicalId":501209,"journal":{"name":"arXiv - PHYS - Earth and Planetary Astrophysics","volume":"8 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142263885","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Rogerio Deienno, Larry Denneau, David Nesvorný, David Vokrouhlický, William F. Bottke, Robert Jedicke, Shantanu Naidu, Steven R. Chesley, Davide Farnocchia, Paul W. Chodas
This work is dedicated to debias the Near-Earth Objects (NEO) population based on observations from the Asteroid Terrestrial-impact Last Alert System (ATLAS) telescopes. We have applied similar methods used to develop the recently released NEO model generator (NEOMOD), once debiasing the NEO population using data from Catalina Sky Survey (CSS) G96 telescope. ATLAS is composed of four different telescopes. We first analyzed observational data from each of all four telescopes separately and later combined them. Our results highlight main differences between CSS and ATLAS, e.g., sky coverage and survey power at debiasing the NEO population. ATLAS has a much larger sky coverage than CSS, allowing it to find bright NEOs that would be constantly "hiding" from CSS. Consequently, ATLAS is more powerful than CSS at debiasing the NEO population for H $lesssim$ 19. With its intrinsically greater sensitivity and emphasis on observing near opposition, CSS excels in the debiasing of smaller objects. ATLAS, as an all sky survey designed to find imminent hazardous objects, necessarily spends a significant fraction of time looking at places on the sky where objects do not appear, reducing its power for debiasing the population of small objects. We estimate a NEO population completeness of $approx$ 88%$^{+3%}_{-2%}$ for H $<$ 17.75 and $approx$ 36%$^{+1%}_{-1%}$ for H $<$ 22.25. Those numbers are similar to previous estimates (within error bars for H $<$ 17.75) from CSS, yet, around 3% and 8% smaller at their face values, respectively. We also confirm previous finding that the $nu_6$ secular resonance is the main source of small and faint NEOs at H = 28, whereas the 3:1 mean motion resonance with Jupiter dominates for larger and brighter NEOs at H = 15.
{"title":"The Debiased Near-Earth Object Population from ATLAS Telescopes","authors":"Rogerio Deienno, Larry Denneau, David Nesvorný, David Vokrouhlický, William F. Bottke, Robert Jedicke, Shantanu Naidu, Steven R. Chesley, Davide Farnocchia, Paul W. Chodas","doi":"arxiv-2409.10453","DOIUrl":"https://doi.org/arxiv-2409.10453","url":null,"abstract":"This work is dedicated to debias the Near-Earth Objects (NEO) population\u0000based on observations from the Asteroid Terrestrial-impact Last Alert System\u0000(ATLAS) telescopes. We have applied similar methods used to develop the\u0000recently released NEO model generator (NEOMOD), once debiasing the NEO\u0000population using data from Catalina Sky Survey (CSS) G96 telescope. ATLAS is\u0000composed of four different telescopes. We first analyzed observational data\u0000from each of all four telescopes separately and later combined them. Our\u0000results highlight main differences between CSS and ATLAS, e.g., sky coverage\u0000and survey power at debiasing the NEO population. ATLAS has a much larger sky\u0000coverage than CSS, allowing it to find bright NEOs that would be constantly\u0000\"hiding\" from CSS. Consequently, ATLAS is more powerful than CSS at debiasing\u0000the NEO population for H $lesssim$ 19. With its intrinsically greater\u0000sensitivity and emphasis on observing near opposition, CSS excels in the\u0000debiasing of smaller objects. ATLAS, as an all sky survey designed to find\u0000imminent hazardous objects, necessarily spends a significant fraction of time\u0000looking at places on the sky where objects do not appear, reducing its power\u0000for debiasing the population of small objects. We estimate a NEO population\u0000completeness of $approx$ 88%$^{+3%}_{-2%}$ for H $<$ 17.75 and $approx$\u000036%$^{+1%}_{-1%}$ for H $<$ 22.25. Those numbers are similar to previous\u0000estimates (within error bars for H $<$ 17.75) from CSS, yet, around 3% and 8%\u0000smaller at their face values, respectively. We also confirm previous finding\u0000that the $nu_6$ secular resonance is the main source of small and faint NEOs\u0000at H = 28, whereas the 3:1 mean motion resonance with Jupiter dominates for\u0000larger and brighter NEOs at H = 15.","PeriodicalId":501209,"journal":{"name":"arXiv - PHYS - Earth and Planetary Astrophysics","volume":"18 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142263893","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Nicholas Scarsdale, C. E. Harman, Thomas J. Fauchez
New observational facilities are beginning to enable insights into the three-dimensional (3D) nature of exoplanets. Transmission spectroscopy is the most widely used method for characterizing transiting temperate exoplanet's atmospheres, but because it only provides a glimpse of the planet's limb and nightside for a typical orbit, its ability to probe 3D characteristics is still an active area of research. Here, we use the ROCKE-3D general circulation model to test the impact of rotation rate, a ``low-order'' 3D characteristic previously shown to drive differences in planetary phase curves, on the transmission spectrum of a representative super-Earth across temperate-to-warm instellations (S$_p$=0.8, 1, 1.25, 1.66, 2, 2.5, 3, 4, 4.56 S$_oplus$). We find that different rotation regimes do display differences in their transmission spectra, primarily driven by clouds and humidity, and that the differences shrink or disappear in hotter regimes where water clouds are unable to condense (though our simulations do not consider haze formation). The small size of the feature differences and potential for degeneracy with other properties, like differing water content or atmospheric structure, mean that we do not specifically claim to have identified a single transmission diagnostic for rotation rate, but our results can be used for holistic spectrum interpretation and sample creation, and suggest the need for more modelling in this area.
{"title":"The Spin Zone: Synchronously and Asynchronously Rotating Exoplanets Have Spectral Differences in Transmission","authors":"Nicholas Scarsdale, C. E. Harman, Thomas J. Fauchez","doi":"arxiv-2409.10752","DOIUrl":"https://doi.org/arxiv-2409.10752","url":null,"abstract":"New observational facilities are beginning to enable insights into the\u0000three-dimensional (3D) nature of exoplanets. Transmission spectroscopy is the\u0000most widely used method for characterizing transiting temperate exoplanet's\u0000atmospheres, but because it only provides a glimpse of the planet's limb and\u0000nightside for a typical orbit, its ability to probe 3D characteristics is still\u0000an active area of research. Here, we use the ROCKE-3D general circulation model\u0000to test the impact of rotation rate, a ``low-order'' 3D characteristic\u0000previously shown to drive differences in planetary phase curves, on the\u0000transmission spectrum of a representative super-Earth across temperate-to-warm\u0000instellations (S$_p$=0.8, 1, 1.25, 1.66, 2, 2.5, 3, 4, 4.56 S$_oplus$). We\u0000find that different rotation regimes do display differences in their\u0000transmission spectra, primarily driven by clouds and humidity, and that the\u0000differences shrink or disappear in hotter regimes where water clouds are unable\u0000to condense (though our simulations do not consider haze formation). The small\u0000size of the feature differences and potential for degeneracy with other\u0000properties, like differing water content or atmospheric structure, mean that we\u0000do not specifically claim to have identified a single transmission diagnostic\u0000for rotation rate, but our results can be used for holistic spectrum\u0000interpretation and sample creation, and suggest the need for more modelling in\u0000this area.","PeriodicalId":501209,"journal":{"name":"arXiv - PHYS - Earth and Planetary Astrophysics","volume":"8 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142263743","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Our Solar System includes the Sun, eight major planets and their moons, along with numerous asteroids, comets, and dust particles, collectively known as the small Solar System bodies. Small bodies are relics from the birth of the Solar System and offer valuable insights into planetary formation and the origins of life. This chapter explores this important component of our Solar System, discussing the formation and evolution of key small body populations and their interrelations.
{"title":"Minor planets, asteroids, comets and interplanetary dust within 30 au","authors":"Quanzhi Ye","doi":"arxiv-2409.09540","DOIUrl":"https://doi.org/arxiv-2409.09540","url":null,"abstract":"Our Solar System includes the Sun, eight major planets and their moons, along\u0000with numerous asteroids, comets, and dust particles, collectively known as the\u0000small Solar System bodies. Small bodies are relics from the birth of the Solar\u0000System and offer valuable insights into planetary formation and the origins of\u0000life. This chapter explores this important component of our Solar System,\u0000discussing the formation and evolution of key small body populations and their\u0000interrelations.","PeriodicalId":501209,"journal":{"name":"arXiv - PHYS - Earth and Planetary Astrophysics","volume":"6 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142263886","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Oliver Shorttle, Homa Saeidfirozeh, Paul Rimmer, Vojtĕch Laitl, Petr Kubelík, Lukáš Petera, Martin Ferus
Intense bombardment of solar system planets in the immediate aftermath of protoplanetary disk dissipation has played a key role in their atmospheric evolution. During this epoch, energetic collisions will have removed significant masses of gas from rocky planet atmospheres. Noble gases are powerful tracers of this early atmospheric history, xenon in particular, which on Mars and Earth shows significant depletions and isotopic fractionations relative to the lighter noble gasses. To evaluate the effect of impacts on the loss and fractionation of xenon, we measure its ionization and recombination efficiency by laser shock and apply these constraints to model impact-driven atmospheric escape on Mars. We demonstrate that impact bombardment within the first $200$ to $300,text{Myr}$ of solar system history generates the observed Xe depletion and isotope fractionation of the modern martian atmosphere. This process may also explain the Xe depletion recorded in Earth's deep mantle and provides a latest date for the timing of giant planet instability.
{"title":"Impact sculpting of the early martian atmosphere","authors":"Oliver Shorttle, Homa Saeidfirozeh, Paul Rimmer, Vojtĕch Laitl, Petr Kubelík, Lukáš Petera, Martin Ferus","doi":"arxiv-2409.07876","DOIUrl":"https://doi.org/arxiv-2409.07876","url":null,"abstract":"Intense bombardment of solar system planets in the immediate aftermath of\u0000protoplanetary disk dissipation has played a key role in their atmospheric\u0000evolution. During this epoch, energetic collisions will have removed\u0000significant masses of gas from rocky planet atmospheres. Noble gases are\u0000powerful tracers of this early atmospheric history, xenon in particular, which\u0000on Mars and Earth shows significant depletions and isotopic fractionations\u0000relative to the lighter noble gasses. To evaluate the effect of impacts on the\u0000loss and fractionation of xenon, we measure its ionization and recombination\u0000efficiency by laser shock and apply these constraints to model impact-driven\u0000atmospheric escape on Mars. We demonstrate that impact bombardment within the\u0000first $200$ to $300,text{Myr}$ of solar system history generates the observed\u0000Xe depletion and isotope fractionation of the modern martian atmosphere. This\u0000process may also explain the Xe depletion recorded in Earth's deep mantle and\u0000provides a latest date for the timing of giant planet instability.","PeriodicalId":501209,"journal":{"name":"arXiv - PHYS - Earth and Planetary Astrophysics","volume":"17 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142204553","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Guang-Yao Xiao, Fabo Feng, Stephen A. Shectman, C. G. Tinney, Johanna K. Teske, B. D. Carter, H. R. A. Jones, Robert A. Wittenmyer, Matías R. Díaz, Jeffrey D. Crane, Sharon X. Wang, J. Bailey, S. J. O'Toole, Adina D. Feinstein, Malena Rice, Zahra Essack, Benjamin T. Montet, Avi Shporer, R. Paul Butler
Giant planets on long period orbits around the nearest stars are among the easiest to directly image. Unfortunately these planets are difficult to fully constrain by indirect methods, e.g., transit and radial velocity (RV). In this study, we present the discovery of a super-Jupiter, HD 222237 b, orbiting a star located $11.445pm0.002$ pc away. By combining RV data, Hipparcos and multi-epoch Gaia astrometry, we estimate the planetary mass to be ${5.19}_{-0.58}^{+0.58},M_{rm Jup}$, with an eccentricity of ${0.56}_{-0.03}^{+0.03}$ and a period of ${40.8}_{-4.5}^{+5.8}$ yr, making HD 222237 b a promising target for imaging using the Mid-Infrared Instrument (MIRI) of JWST. A comparative analysis suggests that our method can break the inclination degeneracy and thus differentiate between prograde and retrograde orbits of a companion. We further find that the inferred contrast ratio between the planet and the host star in the F1550C filter ($15.50,mu rm m$) is approximately $1.9times10^{-4}$, which is comparable with the measured limit of the MIRI coronagraphs. The relatively low metallicity of the host star ($rm-0.32,dex$) combined with the unique orbital architecture of this system presents an excellent opportunity to probe the planet-metallicity correlation and the formation scenarios of giant planets.
围绕最近恒星的长周期轨道上的巨行星是最容易直接成像的。遗憾的是，这些行星很难用间接方法（如凌日和径向速度）来完全约束。在这项研究中，我们发现了一颗超级木星HD 222237 b，它围绕着距离我们11.445/pm0.002$ pc的恒星运行。通过结合RV数据、Hipparcos和多表位Gaia天体测量数据，我们估计这颗行星的质量为${5.19}_{-0.58}^{+0.58},M_{/rm Jup}$，偏心率为${0.56}_{-0.03}^{+0.03}$和周期为${40.8}_{-4.5}^{+5.8}$年，这使得HD222237 b很有希望成为利用JWST的中红外仪器（MIRI）进行成像的目标。对比分析表明，我们的方法可以打破倾角退化，从而区分伴星的顺行和逆行轨道。我们进一步发现，在F1550C滤光片（$15.50, mu rm m$）中，推断出的行星与主星之间的对比度约为1.9times10^{-4}$，这与MIRI日冕仪的测量极限相当。宿主恒星相对较低的金属性（$rm-0.32,dex$）与该系统独特的轨道结构相结合，为探测行星与金属性的相关性以及巨行星的形成情况提供了一个极好的机会。
{"title":"HD 222237 b: a long period super-Jupiter around a nearby star revealed by radial-velocity and Hipparcos-Gaia astrometry","authors":"Guang-Yao Xiao, Fabo Feng, Stephen A. Shectman, C. G. Tinney, Johanna K. Teske, B. D. Carter, H. R. A. Jones, Robert A. Wittenmyer, Matías R. Díaz, Jeffrey D. Crane, Sharon X. Wang, J. Bailey, S. J. O'Toole, Adina D. Feinstein, Malena Rice, Zahra Essack, Benjamin T. Montet, Avi Shporer, R. Paul Butler","doi":"arxiv-2409.08067","DOIUrl":"https://doi.org/arxiv-2409.08067","url":null,"abstract":"Giant planets on long period orbits around the nearest stars are among the\u0000easiest to directly image. Unfortunately these planets are difficult to fully\u0000constrain by indirect methods, e.g., transit and radial velocity (RV). In this\u0000study, we present the discovery of a super-Jupiter, HD 222237 b, orbiting a\u0000star located $11.445pm0.002$ pc away. By combining RV data, Hipparcos and\u0000multi-epoch Gaia astrometry, we estimate the planetary mass to be\u0000${5.19}_{-0.58}^{+0.58},M_{rm Jup}$, with an eccentricity of\u0000${0.56}_{-0.03}^{+0.03}$ and a period of ${40.8}_{-4.5}^{+5.8}$ yr, making HD\u0000222237 b a promising target for imaging using the Mid-Infrared Instrument\u0000(MIRI) of JWST. A comparative analysis suggests that our method can break the\u0000inclination degeneracy and thus differentiate between prograde and retrograde\u0000orbits of a companion. We further find that the inferred contrast ratio between\u0000the planet and the host star in the F1550C filter ($15.50,mu rm m$) is\u0000approximately $1.9times10^{-4}$, which is comparable with the measured limit\u0000of the MIRI coronagraphs. The relatively low metallicity of the host star\u0000($rm-0.32,dex$) combined with the unique orbital architecture of this system\u0000presents an excellent opportunity to probe the planet-metallicity correlation\u0000and the formation scenarios of giant planets.","PeriodicalId":501209,"journal":{"name":"arXiv - PHYS - Earth and Planetary Astrophysics","volume":"11 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142204552","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
The vertical shear instability (VSI) is widely believed to be effective in driving turbulence in protoplanetary disks. Prior studies on VSI exclusively exploit the reflecting boundary conditions (BCs) at the disk surfaces. VSI depends critically on the boundary behaviors of waves at the disk surfaces. We extend earlier studies by performing a comprehensive numerical analysis of VSI with partially reflecting BCs for both the axisymmetric and non-axisymmetric unstable VSI modes. We find that the growth rates of the unstable modes diminish when the outgoing component of the flow is greater than the incoming one for high-order body modes. When the outgoing wave component dominates, the growth of VSI is notably suppressed. We find that the non-axisymmetric modes are unstable and they grow at a rate that decreases with the azimuthal wavenumber. The different BCs at the lower and upper disk surfaces naturally lead to non-symmetric modes relative to the disk midplane. The potential implications of our studies for further understanding planetary formation and evolution in protoplanetary disks (PPDs) are also briefly discussed.
人们普遍认为垂直剪切不稳定性（VSI）能有效地驱动原行星盘中的湍流。先前关于VSI的研究只利用了盘面的反射边界条件（BCs）。VSI关键取决于圆盘表面波的边界行为。我们扩展了之前的研究，对轴对称和非轴对称不稳定 VSI 模式的部分反射边界条件进行了全面的数值分析。我们发现，对于高阶体模而言，当流出分量大于流入分量时，不稳定模的增长率会减小。当流出波分量占主导地位时，VSI 的增长明显受到抑制。我们发现，非轴对称模态是不稳定的，它们的增长速度随方位角波数的增加而减小。圆盘下表面和上表面的 BC 不同，自然会导致相对于圆盘中平面的非对称模式。此外，还简要讨论了我们的研究对进一步理解原行星盘中行星形成和演化的潜在影响。
{"title":"Vertical Shear Instability with Partially Reflecting Boundary Conditions","authors":"Yuzi Wu, Cong Yu, Can Cui","doi":"arxiv-2409.07898","DOIUrl":"https://doi.org/arxiv-2409.07898","url":null,"abstract":"The vertical shear instability (VSI) is widely believed to be effective in\u0000driving turbulence in protoplanetary disks. Prior studies on VSI exclusively\u0000exploit the reflecting boundary conditions (BCs) at the disk surfaces. VSI\u0000depends critically on the boundary behaviors of waves at the disk surfaces. We\u0000extend earlier studies by performing a comprehensive numerical analysis of VSI\u0000with partially reflecting BCs for both the axisymmetric and non-axisymmetric\u0000unstable VSI modes. We find that the growth rates of the unstable modes\u0000diminish when the outgoing component of the flow is greater than the incoming\u0000one for high-order body modes. When the outgoing wave component dominates, the\u0000growth of VSI is notably suppressed. We find that the non-axisymmetric modes\u0000are unstable and they grow at a rate that decreases with the azimuthal\u0000wavenumber. The different BCs at the lower and upper disk surfaces naturally\u0000lead to non-symmetric modes relative to the disk midplane. The potential\u0000implications of our studies for further understanding planetary formation and\u0000evolution in protoplanetary disks (PPDs) are also briefly discussed.","PeriodicalId":501209,"journal":{"name":"arXiv - PHYS - Earth and Planetary Astrophysics","volume":"316 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142226169","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
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