Upcoming large multiwavelength photometric surveys will provide a leap in our understanding of small body populations, among other fields of modern astrophysics. Serendipitous observations of small bodies in different orbital locations allow us to study diverse phenomena related to how their surfaces scatter solar light. In particular, multiple observations of the same object in different epochs permit us to construct their phase curves to obtain absolute magnitudes and phase coefficients. In this work, we tackle a series of long-used relationships associating these phase coefficients with the taxa of small bodies and suggest that some may need to be revised in the light of large-number statistics.
{"title":"A discussion on estimating small bodies taxonomies using phase curves results","authors":"Alvaro Alvarez-Candal","doi":"arxiv-2409.05775","DOIUrl":"https://doi.org/arxiv-2409.05775","url":null,"abstract":"Upcoming large multiwavelength photometric surveys will provide a leap in our\u0000understanding of small body populations, among other fields of modern\u0000astrophysics. Serendipitous observations of small bodies in different orbital\u0000locations allow us to study diverse phenomena related to how their surfaces\u0000scatter solar light. In particular, multiple observations of the same object in different epochs\u0000permit us to construct their phase curves to obtain absolute magnitudes and\u0000phase coefficients. In this work, we tackle a series of long-used relationships\u0000associating these phase coefficients with the taxa of small bodies and suggest\u0000that some may need to be revised in the light of large-number statistics.","PeriodicalId":501209,"journal":{"name":"arXiv - PHYS - Earth and Planetary Astrophysics","volume":"50 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142204592","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}
Apophis' current trajectory takes it safely past our planet at a distance of several Earth radii on 2029 April 13. Here the possibility is considered that Apophis could collide with a small asteroid, like the ones that frequently and unpredictably strike Earth, and the resulting perturbation of its trajectory. The probability of an impact that could significantly displace Apophis relative to its keyholes is found to be less than 1 in $10^6$, requiring a delta-v greater than 0.3 mm/s, while for an impact that could significantly displace Apophis compared to its miss distance in 2029 it is less than 1 in $10^9$, requiring a delta-v greater than 5 cm/s. These probabilities are below the usual thresholds considered by asteroid impact warning systems. Apophis is in the daytime sky and unobservable from mid-2021 to 2027. It will be challenging to determine from single night observations in 2027 if Apophis has moved on the target plane enough to enter a dangerous keyhole, as the deviation from the nominal ephemeris might be only a few tenths of an arcsecond. An impending Earth impact would, however, be signalled clearly in most cases by deviations of tens of arcseconds of Apophis from its nominal ephemeris in 2027. Thus most of the impact risk could be retired by a single observation of Apophis in 2027, though a minority of cases present some ambiguity and are discussed in more detail. Charts of the on-sky position of Apophis under different scenarios are presented for quick assessment by observers.
{"title":"On the sensitivity of Apophis' 2029 Earth approach to small asteroid impacts","authors":"Paul Wiegert","doi":"arxiv-2409.06059","DOIUrl":"https://doi.org/arxiv-2409.06059","url":null,"abstract":"Apophis' current trajectory takes it safely past our planet at a distance of\u0000several Earth radii on 2029 April 13. Here the possibility is considered that\u0000Apophis could collide with a small asteroid, like the ones that frequently and\u0000unpredictably strike Earth, and the resulting perturbation of its trajectory.\u0000The probability of an impact that could significantly displace Apophis relative\u0000to its keyholes is found to be less than 1 in $10^6$, requiring a delta-v\u0000greater than 0.3 mm/s, while for an impact that could significantly displace\u0000Apophis compared to its miss distance in 2029 it is less than 1 in $10^9$,\u0000requiring a delta-v greater than 5 cm/s. These probabilities are below the\u0000usual thresholds considered by asteroid impact warning systems. Apophis is in the daytime sky and unobservable from mid-2021 to 2027. It will\u0000be challenging to determine from single night observations in 2027 if Apophis\u0000has moved on the target plane enough to enter a dangerous keyhole, as the\u0000deviation from the nominal ephemeris might be only a few tenths of an\u0000arcsecond. An impending Earth impact would, however, be signalled clearly in\u0000most cases by deviations of tens of arcseconds of Apophis from its nominal\u0000ephemeris in 2027. Thus most of the impact risk could be retired by a single\u0000observation of Apophis in 2027, though a minority of cases present some\u0000ambiguity and are discussed in more detail. Charts of the on-sky position of\u0000Apophis under different scenarios are presented for quick assessment by\u0000observers.","PeriodicalId":501209,"journal":{"name":"arXiv - PHYS - Earth and Planetary Astrophysics","volume":"23 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142204589","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}
High-resolution millimetre-imaging of protoplanetary discs has revealed many containing rings and gaps. These rings can contain large quantities of dust, often in excess of 10M$_oplus$, providing prime sites for efficient and rapid planet formation. Rapid planet formation will produce high accretion luminosities, heating the surrounding disc. We investigate the importance of a planetary embryo's accretion luminosity by simulating the dynamics of the gas and dust in a dust ring, accounting for the energy liberated as a resident planetary embryo accretes. The resulting heating alters the flow structure near the planet, increasing the accretion rate of large, millimetre-to-centimetre-sized dust grains. We show how this process varies with the mass of dust in the ring and the local background gas temperature, demonstrating that the thermal feedback always acts to increase the planet's mass. This increase in planet mass is driven primarily by the formation of vortices, created by a baroclinic instability once the accreting planet heats the disc significantly outside its Hill radius. The vortices can then migrate with respect to the planet, resulting in a complex interplay between planetary growth, gap-opening, dust trapping and vortex dynamics. Planets formed within dust traps can have masses that exceed the classical pebble isolation mass, potentially providing massive seeds for the future formation of giant planets. Once pebble accretion ceases, the local dust size distribution is depleted in large grains, and much of the remaining dust mass is trapped in the system's L$_5$ Lagrange point, providing potentially observable signatures of this evolution.
{"title":"The Role of Thermal Feedback in the Growth of Planetary Cores by Pebble Accretion in Dust Traps","authors":"Daniel P. Cummins, James E. Owen","doi":"arxiv-2409.05951","DOIUrl":"https://doi.org/arxiv-2409.05951","url":null,"abstract":"High-resolution millimetre-imaging of protoplanetary discs has revealed many\u0000containing rings and gaps. These rings can contain large quantities of dust,\u0000often in excess of 10M$_oplus$, providing prime sites for efficient and rapid\u0000planet formation. Rapid planet formation will produce high accretion\u0000luminosities, heating the surrounding disc. We investigate the importance of a\u0000planetary embryo's accretion luminosity by simulating the dynamics of the gas\u0000and dust in a dust ring, accounting for the energy liberated as a resident\u0000planetary embryo accretes. The resulting heating alters the flow structure near\u0000the planet, increasing the accretion rate of large,\u0000millimetre-to-centimetre-sized dust grains. We show how this process varies\u0000with the mass of dust in the ring and the local background gas temperature,\u0000demonstrating that the thermal feedback always acts to increase the planet's\u0000mass. This increase in planet mass is driven primarily by the formation of\u0000vortices, created by a baroclinic instability once the accreting planet heats\u0000the disc significantly outside its Hill radius. The vortices can then migrate\u0000with respect to the planet, resulting in a complex interplay between planetary\u0000growth, gap-opening, dust trapping and vortex dynamics. Planets formed within\u0000dust traps can have masses that exceed the classical pebble isolation mass,\u0000potentially providing massive seeds for the future formation of giant planets.\u0000Once pebble accretion ceases, the local dust size distribution is depleted in\u0000large grains, and much of the remaining dust mass is trapped in the system's\u0000L$_5$ Lagrange point, providing potentially observable signatures of this\u0000evolution.","PeriodicalId":501209,"journal":{"name":"arXiv - PHYS - Earth and Planetary Astrophysics","volume":"4 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142226170","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}
M. A. Cordiner, K. Darnell, D. Bockeleé-Morvan, N. X. Roth, N. Biver, S. N. Milam, S. B. Charnley, J. Boissier, B. P. Bonev, C. Qi, J. Crovisier, A. J. Remijan
46P/Wirtanen is a Jupiter-family comet, probably originating from the Solar System's Kuiper belt, that now resides on a 5.4 year elliptical orbit. During its 2018 apparition, comet 46P passed unusually close to the Earth (within 0.08 au), presenting an outstanding opportunity for close-up observations of its inner coma. Here we present observations of HCN, H$^{13}$CN and HC$^{15}$N emission from 46P using the Atacama Compact Array (ACA). The data were analyzed using the SUBLIME non-LTE radiative transfer code to derive $^{12}$C/$^{13}$C and $^{14}$N/$^{15}$N ratios. The HCN/H$^{13}$CN ratio is found to be consistent with a lack of significant $^{13}$C fractionation, whereas the HCN/HC$^{15}$N ratio of $68pm27$ (using our most conservative $1sigma$ uncertainties), indicates a strong enhancement in $^{15}$N compared with the solar and terrestrial values. The observed $^{14}$N/$^{15}$N ratio is also significantly lower than the values of $sim140$ found in previous comets, implying a strong $^{15}$N enrichment in 46P's HCN. This indicates that the nitrogen in Jupiter-family comets could reach larger isotopic enrichments than previously thought, with implications for the diversity of $^{14}$N/$^{15}$N ratios imprinted into icy bodies at the birth of the Solar System.
{"title":"Evidence for Surprising Heavy Nitrogen Isotopic Enrichment in Comet 46P/Wirtanen's Hydrogen Cyanide","authors":"M. A. Cordiner, K. Darnell, D. Bockeleé-Morvan, N. X. Roth, N. Biver, S. N. Milam, S. B. Charnley, J. Boissier, B. P. Bonev, C. Qi, J. Crovisier, A. J. Remijan","doi":"arxiv-2409.05711","DOIUrl":"https://doi.org/arxiv-2409.05711","url":null,"abstract":"46P/Wirtanen is a Jupiter-family comet, probably originating from the Solar\u0000System's Kuiper belt, that now resides on a 5.4 year elliptical orbit. During\u0000its 2018 apparition, comet 46P passed unusually close to the Earth (within 0.08\u0000au), presenting an outstanding opportunity for close-up observations of its\u0000inner coma. Here we present observations of HCN, H$^{13}$CN and HC$^{15}$N\u0000emission from 46P using the Atacama Compact Array (ACA). The data were analyzed\u0000using the SUBLIME non-LTE radiative transfer code to derive $^{12}$C/$^{13}$C\u0000and $^{14}$N/$^{15}$N ratios. The HCN/H$^{13}$CN ratio is found to be\u0000consistent with a lack of significant $^{13}$C fractionation, whereas the\u0000HCN/HC$^{15}$N ratio of $68pm27$ (using our most conservative $1sigma$\u0000uncertainties), indicates a strong enhancement in $^{15}$N compared with the\u0000solar and terrestrial values. The observed $^{14}$N/$^{15}$N ratio is also\u0000significantly lower than the values of $sim140$ found in previous comets,\u0000implying a strong $^{15}$N enrichment in 46P's HCN. This indicates that the\u0000nitrogen in Jupiter-family comets could reach larger isotopic enrichments than\u0000previously thought, with implications for the diversity of $^{14}$N/$^{15}$N\u0000ratios imprinted into icy bodies at the birth of the Solar System.","PeriodicalId":501209,"journal":{"name":"arXiv - PHYS - Earth and Planetary Astrophysics","volume":"20 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142226171","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}
Stability of Hilda Asteroids in the solar system around the 3:2 resonance point is analyzed in terms of the Sun-Jupiter-asteroid elliptic restricted three-body problem. We show that the Hamiltonian of the system is well-approximated by a single-resonance Hamiltonian around the 3:2 resonance. This implies that orbits of the Hilda asteroids are approximately integrable, thus their motion is stable. This is in contrast to other resonances such as the 3:1 and the 2:1 resonances at which Kirkwood gaps occur. Indeed, around the 3:1 and the 2:1 resonances, the Hamiltonians are approximated by double-resonance Hamiltonians that are nonintegrable and thus indicate chaotic motions. By a suitable canonical transformation, we reduce the number of degrees of freedom for the system and derive a Hamiltonian which has two degrees of freedom. As a result, we can analyze the stability of the motion by constructing Poincare surface of section.
{"title":"Stability of Hilda asteroids at 3:2 resonance point in restricted three-body problem","authors":"Kosuke Asano, Kenichi Noba, Tomio Petrosky","doi":"arxiv-2409.05102","DOIUrl":"https://doi.org/arxiv-2409.05102","url":null,"abstract":"Stability of Hilda Asteroids in the solar system around the 3:2 resonance\u0000point is analyzed in terms of the Sun-Jupiter-asteroid elliptic restricted\u0000three-body problem. We show that the Hamiltonian of the system is\u0000well-approximated by a single-resonance Hamiltonian around the 3:2 resonance.\u0000This implies that orbits of the Hilda asteroids are approximately integrable,\u0000thus their motion is stable. This is in contrast to other resonances such as\u0000the 3:1 and the 2:1 resonances at which Kirkwood gaps occur. Indeed, around the\u00003:1 and the 2:1 resonances, the Hamiltonians are approximated by\u0000double-resonance Hamiltonians that are nonintegrable and thus indicate chaotic\u0000motions. By a suitable canonical transformation, we reduce the number of\u0000degrees of freedom for the system and derive a Hamiltonian which has two\u0000degrees of freedom. As a result, we can analyze the stability of the motion by\u0000constructing Poincare surface of section.","PeriodicalId":501209,"journal":{"name":"arXiv - PHYS - Earth and Planetary Astrophysics","volume":"12 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142204594","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}
Efrain Alvarado III, Kate B. Bostow, Kishore C. Patra, Cooper H. Jacobus, Raphael A. Baer-Way, Connor F. Jennings, Neil R. Pichay, Asia A. deGraw, Edgar P. Vidal, Vidhi Chander, Ivan A. Altunin, Victoria M. Brendel, Kingsley E. Ehrich, James D. Sunseri, Michael B. May, Druv H. Punjabi, Eli A. Gendreau-Distler, Sophia Risin, Thomas G. Brink, WeiKang Zheng, Alexei V. Filippenko
We study transits of several ``hot Jupiter'' systems - including WASP-12 b, WASP-43 b, WASP-103 b, HAT-P-23 b, KELT-16 b, WD 1856+534 b, and WTS-2 b - with the goal of detecting tidal orbital decay and extending the baselines of transit times. We find no evidence of orbital decay in any of the observed systems except for that of the extensively studied WASP-12 b. Although the orbit of WASP-12 b is unequivocally decaying, we find no evidence for acceleration of said orbital decay, with measured $ddot{P} = (-7 pm 8) times 10^{-14} rm ~s^{-1}$, against the expected acceleration decay of $ddot{P} approx -10^{-23} rm ~s^{-1}$. In the case of WD 1856+534 b, there is a tentative detection of orbital growth with $dot{P} = (5.0 pm 1.5) times 10^{-10}$. While statistically significant, we err on the side of caution and wait for longer follow-up observations to consider the measured $dot{P}$ real. For most systems, we provide a 95%-confidence lower limit on the tidal quality factor, $Q_star'$. The possibility of detecting orbital decay in hot Jupiters via long-term radial velocity (RV) measurements is also explored. We find that $sim 1 rm ~m~s^{-1}$ precision in RVs will be required to detect orbital decay of WASP-12 b with only 3 yr of observations. Currently available RV measurements and precision are unable to detect orbital decay in any of the systems studied here.
{"title":"Searching for Tidal Orbital Decay in Hot Jupiters","authors":"Efrain Alvarado III, Kate B. Bostow, Kishore C. Patra, Cooper H. Jacobus, Raphael A. Baer-Way, Connor F. Jennings, Neil R. Pichay, Asia A. deGraw, Edgar P. Vidal, Vidhi Chander, Ivan A. Altunin, Victoria M. Brendel, Kingsley E. Ehrich, James D. Sunseri, Michael B. May, Druv H. Punjabi, Eli A. Gendreau-Distler, Sophia Risin, Thomas G. Brink, WeiKang Zheng, Alexei V. Filippenko","doi":"arxiv-2409.04660","DOIUrl":"https://doi.org/arxiv-2409.04660","url":null,"abstract":"We study transits of several ``hot Jupiter'' systems - including WASP-12 b,\u0000WASP-43 b, WASP-103 b, HAT-P-23 b, KELT-16 b, WD 1856+534 b, and WTS-2 b - with\u0000the goal of detecting tidal orbital decay and extending the baselines of\u0000transit times. We find no evidence of orbital decay in any of the observed\u0000systems except for that of the extensively studied WASP-12 b. Although the\u0000orbit of WASP-12 b is unequivocally decaying, we find no evidence for\u0000acceleration of said orbital decay, with measured $ddot{P} = (-7 pm 8) times\u000010^{-14} rm ~s^{-1}$, against the expected acceleration decay of $ddot{P}\u0000approx -10^{-23} rm ~s^{-1}$. In the case of WD 1856+534 b, there is a\u0000tentative detection of orbital growth with $dot{P} = (5.0 pm 1.5) times\u000010^{-10}$. While statistically significant, we err on the side of caution and\u0000wait for longer follow-up observations to consider the measured $dot{P}$ real.\u0000For most systems, we provide a 95%-confidence lower limit on the tidal quality\u0000factor, $Q_star'$. The possibility of detecting orbital decay in hot Jupiters\u0000via long-term radial velocity (RV) measurements is also explored. We find that\u0000$sim 1 rm ~m~s^{-1}$ precision in RVs will be required to detect orbital\u0000decay of WASP-12 b with only 3 yr of observations. Currently available RV\u0000measurements and precision are unable to detect orbital decay in any of the\u0000systems studied here.","PeriodicalId":501209,"journal":{"name":"arXiv - PHYS - Earth and Planetary Astrophysics","volume":"30 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142226172","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}
D. Athanasopoulos, J. Hanuš, C. Avdellidou, G. van Belle, A. Ferrero, R. Bonamico, K. Gazeas, M. Delbo, J. P. Rivet, G. Apostolovska, N. Todorović, B. Novakovic, E. V. Bebekovska, Y. Romanyuk, B. T. Bolin, W. Zhou, H. Agrusa
The aim of our study is to characterise the spin states of the members of the Athor and Zita collisional families and test whether these members have a spin distribution consistent with a common origin from the break up of their respective family parent asteroids. Our method is based on the asteroid family evolution, which indicates that there should be a statistical predominance of retrograde-rotating asteroids on the inward side of family's V-shape, and prograde-rotating asteroids on the outward side. We used photometric data from our campaign and the literature in order to reveal the spin states of the asteroids belonging to these families. We combined dense and sparse photometric data in order to construct lightcurves; we performed the lightcurve inversion method to estimate the sidereal period, spin axis and convex shape of several family members. We obtained 34 new asteroid models for Athor family members and 17 for Zita family members. Along with the literature and revised models, the Athor family contains 60% of retrograde asteroids on the inward side and, 76% of prograde asteroids on the outward side. We also found that the Zita family exhibits 80% of retrograde asteroids on the inward side and an equal amount of prograde and retrograde rotators on the outward side. However, when we applied Kernel density estimation, we also found a clear peak for prograde asteroids on the outward side, as expected from the theory. The spin states of these asteroids validate the existence of both families, with the Athor family exhibiting a stronger signature for the presence of retrograde-rotating and prograde-rotating asteroids on the inner and outer side of the family, respectively. Our work provides an independent confirmation and characterisation of these very old families, whose presence and characteristics offer constraints for theories and models of the Solar System's evolution.
{"title":"Spin states of X-complex asteroids in the inner main belt -- I. Investigating the Athor and Zita collisional families","authors":"D. Athanasopoulos, J. Hanuš, C. Avdellidou, G. van Belle, A. Ferrero, R. Bonamico, K. Gazeas, M. Delbo, J. P. Rivet, G. Apostolovska, N. Todorović, B. Novakovic, E. V. Bebekovska, Y. Romanyuk, B. T. Bolin, W. Zhou, H. Agrusa","doi":"arxiv-2409.03419","DOIUrl":"https://doi.org/arxiv-2409.03419","url":null,"abstract":"The aim of our study is to characterise the spin states of the members of the\u0000Athor and Zita collisional families and test whether these members have a spin\u0000distribution consistent with a common origin from the break up of their\u0000respective family parent asteroids. Our method is based on the asteroid family\u0000evolution, which indicates that there should be a statistical predominance of\u0000retrograde-rotating asteroids on the inward side of family's V-shape, and\u0000prograde-rotating asteroids on the outward side. We used photometric data from\u0000our campaign and the literature in order to reveal the spin states of the\u0000asteroids belonging to these families. We combined dense and sparse photometric\u0000data in order to construct lightcurves; we performed the lightcurve inversion\u0000method to estimate the sidereal period, spin axis and convex shape of several\u0000family members. We obtained 34 new asteroid models for Athor family members and\u000017 for Zita family members. Along with the literature and revised models, the\u0000Athor family contains 60% of retrograde asteroids on the inward side and, 76%\u0000of prograde asteroids on the outward side. We also found that the Zita family\u0000exhibits 80% of retrograde asteroids on the inward side and an equal amount of\u0000prograde and retrograde rotators on the outward side. However, when we applied\u0000Kernel density estimation, we also found a clear peak for prograde asteroids on\u0000the outward side, as expected from the theory. The spin states of these\u0000asteroids validate the existence of both families, with the Athor family\u0000exhibiting a stronger signature for the presence of retrograde-rotating and\u0000prograde-rotating asteroids on the inner and outer side of the family,\u0000respectively. Our work provides an independent confirmation and\u0000characterisation of these very old families, whose presence and characteristics\u0000offer constraints for theories and models of the Solar System's evolution.","PeriodicalId":501209,"journal":{"name":"arXiv - PHYS - Earth and Planetary Astrophysics","volume":"1 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142204612","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}
Frances E. Rigby, Lorenzo Pica-Ciamarra, Måns Holmberg, Nikku Madhusudhan, Savvas Constantinou, Laura Schaefer, Jie Deng, Kanani K. M. Lee, Julianne I. Moses
The recent JWST detections of carbon-bearing molecules in a habitable-zone sub-Neptune have opened a new era in the study of low-mass exoplanets. The sub-Neptune regime spans a wide diversity of planetary interiors and atmospheres not witnessed in the solar system, including mini-Neptunes, super-Earths, and water worlds. Recent works have investigated the possibility of gas dwarfs, with rocky interiors and thick H$_2$-rich atmospheres, to explain aspects of the sub-Neptune population, including the radius valley. Interactions between the H$_2$-rich envelope and a potential magma ocean may lead to observable atmospheric signatures. We report a coupled interior-atmosphere modelling framework for gas dwarfs to investigate the plausibility of magma oceans on such planets and their observable diagnostics. We find that the surface-atmosphere interactions and atmospheric composition are sensitive to a wide range of parameters, including the atmospheric and internal structure, mineral composition, volatile solubility and atmospheric chemistry. While magma oceans are typically associated with high-temperature rocky planets, we assess if such conditions may be admissible and observable for temperate sub-Neptunes. We find that a holistic modelling approach is required for this purpose and to avoid unphysical model solutions. We find using our model framework and considering the habitable-zone sub-Neptune K2-18 b as a case study that its observed atmospheric composition is incompatible with a magma ocean scenario. We identify key atmospheric molecular and elemental diagnostics, including the abundances of CO$_2$, CO, NH$_3$ and, potentially, S-bearing species. Our study also underscores the need for fundamental material properties for accurate modelling of such planets.
最近，JWST 在海王星下宜居带探测到含碳分子，这开启了低质量系外行星研究的新纪元。海王星下轨道涵盖了太阳系中从未见过的多种行星内部和大气层，包括小海王星、超级地球和水世界。最近的工作研究了具有岩石内部和富含H$_2$的厚大气层的气体矮星的可能性，以解释亚海王星群的各个方面，包括半径谷。我们报告了一个气态矮星内部-大气耦合建模框架，以研究这类行星上岩浆海洋的合理性及其可观测诊断。我们发现，表面-大气相互作用和大气成分对一系列参数非常敏感，包括大气和内部结构、矿物成分、挥发性溶解度和大气化学。虽然岩浆海洋通常与高温海王星有关，但我们评估了温带亚海王星是否可能存在和观测到这样的条件。我们发现，为此需要一种整体建模方法，以避免非物理模型解决方案。我们发现，利用我们的模型框架，并将宜居带亚海王星 K2-18b 作为案例研究，其观测到的大气成分与岩浆海洋方案不相容。我们确定了关键的大气分子和元素诊断，包括 CO$_2$、CO、NH$_3$ 以及潜在的含 S 物种的丰度。我们的研究还强调了为此类行星建立精确模型所需的基本物质特性。
{"title":"Towards a self-consistent evaluation of gas dwarf scenarios for temperate sub-Neptunes","authors":"Frances E. Rigby, Lorenzo Pica-Ciamarra, Måns Holmberg, Nikku Madhusudhan, Savvas Constantinou, Laura Schaefer, Jie Deng, Kanani K. M. Lee, Julianne I. Moses","doi":"arxiv-2409.03683","DOIUrl":"https://doi.org/arxiv-2409.03683","url":null,"abstract":"The recent JWST detections of carbon-bearing molecules in a habitable-zone\u0000sub-Neptune have opened a new era in the study of low-mass exoplanets. The\u0000sub-Neptune regime spans a wide diversity of planetary interiors and\u0000atmospheres not witnessed in the solar system, including mini-Neptunes,\u0000super-Earths, and water worlds. Recent works have investigated the possibility\u0000of gas dwarfs, with rocky interiors and thick H$_2$-rich atmospheres, to\u0000explain aspects of the sub-Neptune population, including the radius valley.\u0000Interactions between the H$_2$-rich envelope and a potential magma ocean may\u0000lead to observable atmospheric signatures. We report a coupled\u0000interior-atmosphere modelling framework for gas dwarfs to investigate the\u0000plausibility of magma oceans on such planets and their observable diagnostics.\u0000We find that the surface-atmosphere interactions and atmospheric composition\u0000are sensitive to a wide range of parameters, including the atmospheric and\u0000internal structure, mineral composition, volatile solubility and atmospheric\u0000chemistry. While magma oceans are typically associated with high-temperature\u0000rocky planets, we assess if such conditions may be admissible and observable\u0000for temperate sub-Neptunes. We find that a holistic modelling approach is\u0000required for this purpose and to avoid unphysical model solutions. We find\u0000using our model framework and considering the habitable-zone sub-Neptune K2-18\u0000b as a case study that its observed atmospheric composition is incompatible\u0000with a magma ocean scenario. We identify key atmospheric molecular and\u0000elemental diagnostics, including the abundances of CO$_2$, CO, NH$_3$ and,\u0000potentially, S-bearing species. Our study also underscores the need for\u0000fundamental material properties for accurate modelling of such planets.","PeriodicalId":501209,"journal":{"name":"arXiv - PHYS - Earth and Planetary Astrophysics","volume":"9 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142204609","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}
Javier Rodríguez Rodríguez, Enrique Díez Alonso, Santiago Iglesias Álvarez, Saúl Pérez Fernández, Alejandro Buendia Roca, Julia Fernández Díaz, Javier Licandro, Miguel R. Alarcon, Miquel Serra-Ricart, Noemi Pinilla-Alonso, Francisco Javier de Cos Juez
In an attempt to further characterise the near-Earth asteroid (NEA) population we present 38 new light-curves acquired between September 2020 and November 2023 for NEAs (7335) 1989 JA, (7822) 1991 CS, (154244) 2002 KL6 and (159402) 1999 AP10, obtained from observations taken at the Teide Observatory (Tenerife, Spain). With these new observations along with archival data, we computed their first shape models and spin solutions by applying the light curve inversion method. The obtained rotation periods are in good agreement with those reported in previous works, with improved uncertainties. Additionally, besides the constant period models for (7335) 1989 JA, (7822) 1991 CS and (159402) 1999 AP10, our results for (154244) 2002 KL6 suggest that it could be affected by a Yarkovsky-O'Keefe-Radzievskii-Paddack acceleration with a value of $upsilon simeq -7 times 10^{-9}$ rad d$^{-2}$. This would be one of the first detections of this effect slowing down an asteroid.
{"title":"Light-curve analysis and shape models of NEAs 7335, 7822, 154244 and 159402","authors":"Javier Rodríguez Rodríguez, Enrique Díez Alonso, Santiago Iglesias Álvarez, Saúl Pérez Fernández, Alejandro Buendia Roca, Julia Fernández Díaz, Javier Licandro, Miguel R. Alarcon, Miquel Serra-Ricart, Noemi Pinilla-Alonso, Francisco Javier de Cos Juez","doi":"arxiv-2409.03446","DOIUrl":"https://doi.org/arxiv-2409.03446","url":null,"abstract":"In an attempt to further characterise the near-Earth asteroid (NEA)\u0000population we present 38 new light-curves acquired between September 2020 and\u0000November 2023 for NEAs (7335) 1989 JA, (7822) 1991 CS, (154244) 2002 KL6 and\u0000(159402) 1999 AP10, obtained from observations taken at the Teide Observatory\u0000(Tenerife, Spain). With these new observations along with archival data, we\u0000computed their first shape models and spin solutions by applying the light\u0000curve inversion method. The obtained rotation periods are in good agreement\u0000with those reported in previous works, with improved uncertainties.\u0000Additionally, besides the constant period models for (7335) 1989 JA, (7822)\u00001991 CS and (159402) 1999 AP10, our results for (154244) 2002 KL6 suggest that\u0000it could be affected by a Yarkovsky-O'Keefe-Radzievskii-Paddack acceleration\u0000with a value of $upsilon simeq -7 times 10^{-9}$ rad d$^{-2}$. This would be\u0000one of the first detections of this effect slowing down an asteroid.","PeriodicalId":501209,"journal":{"name":"arXiv - PHYS - Earth and Planetary Astrophysics","volume":"9 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142204611","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}
Context. Dust coagulation and fragmentation impact the structure and evolution of protoplanetary disks and set the initial conditions for planet formation. Dust grains dominate the opacities, they determine the cooling times of the gas, they influence the ionization state of the gas, and the grain surface area is an important parameter for the chemistry in protoplanetary disks. Therefore, dust evolution should not be ignored in numerical studies of protoplanetary disks. Available dust coagulation models are, however, too computationally expensive to be implemented in large-scale hydrodynamic simulations. This limits detailed numerical studies of protoplanetary disks, including these effects, mostly to one-dimensional models. Aims. We aim to develop a simple - yet accurate - dust coagulation model that can be implemented in hydrodynamic simulations of protoplanetary disks. Our model shall not significantly increase the computational cost of simulations and provide information about the local grain size distribution. Methods. The local dust size distributions are assumed to be truncated power laws. Such distributions can be characterized by two dust fluids (large and small grains) and a maximum particle size, truncating the power law. We compare our model to state-of-the-art dust coagulation simulations and calibrate it to achieve a good fit with these sophisticated numerical methods. Results. Running various parameter studies, we achieved a good fit between our simplified three-parameter model and DustPy, a state-of-the-art dust coagulation software. Conclusions. We present TriPoD, a sub-grid dust coagulation model for the PLUTO code. With TriPoD, we can perform two-dimensional, vertically integrated dust coagulation simulations on top of a hydrodynamic simulation. Studying the dust distributions in two-dimensional vortices and planet-disk systems is thus made possible.
{"title":"TriPoD: Tri-Population size distributions for Dust evolution. Coagulation in vertically integrated hydrodynamic simulations of protoplanetary disks","authors":"Thomas Pfeil, Til Birnstiel, Hubert Klahr","doi":"arxiv-2409.03816","DOIUrl":"https://doi.org/arxiv-2409.03816","url":null,"abstract":"Context. Dust coagulation and fragmentation impact the structure and\u0000evolution of protoplanetary disks and set the initial conditions for planet\u0000formation. Dust grains dominate the opacities, they determine the cooling times\u0000of the gas, they influence the ionization state of the gas, and the grain\u0000surface area is an important parameter for the chemistry in protoplanetary\u0000disks. Therefore, dust evolution should not be ignored in numerical studies of\u0000protoplanetary disks. Available dust coagulation models are, however, too\u0000computationally expensive to be implemented in large-scale hydrodynamic\u0000simulations. This limits detailed numerical studies of protoplanetary disks,\u0000including these effects, mostly to one-dimensional models. Aims. We aim to develop a simple - yet accurate - dust coagulation model that\u0000can be implemented in hydrodynamic simulations of protoplanetary disks. Our\u0000model shall not significantly increase the computational cost of simulations\u0000and provide information about the local grain size distribution. Methods. The local dust size distributions are assumed to be truncated power\u0000laws. Such distributions can be characterized by two dust fluids (large and\u0000small grains) and a maximum particle size, truncating the power law. We compare\u0000our model to state-of-the-art dust coagulation simulations and calibrate it to\u0000achieve a good fit with these sophisticated numerical methods. Results. Running various parameter studies, we achieved a good fit between\u0000our simplified three-parameter model and DustPy, a state-of-the-art dust\u0000coagulation software. Conclusions. We present TriPoD, a sub-grid dust coagulation model for the\u0000PLUTO code. With TriPoD, we can perform two-dimensional, vertically integrated\u0000dust coagulation simulations on top of a hydrodynamic simulation. Studying the\u0000dust distributions in two-dimensional vortices and planet-disk systems is thus\u0000made possible.","PeriodicalId":501209,"journal":{"name":"arXiv - PHYS - Earth and Planetary Astrophysics","volume":"64 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142204596","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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