arXiv - PHYS - Earth and Planetary Astrophysics最新文献

{"title":"Impact of vegetation albedo on the habitability of Earth-like exoplanets","authors":"Erica Bisesi, Giuseppe Murante, Antonello Provenzale, Lorenzo Biasiotti, Jost von Hardenberg, Stavro Ivanovski, Michele Maris, Sergio Monai, Laura Silva, Paolo Simonetti, Giovanni Vladilo","doi":"arxiv-2409.01746","DOIUrl":"https://doi.org/arxiv-2409.01746","url":null,"abstract":"Vegetation can modify the planetary surface albedo via the Charney mechanism,\u0000as plants are usually darker than the bare surface of the continents. We\u0000updated ESTM (Earth-like Surface Temperature Model) to incorporate the\u0000presence, distribution and evolution of two dynamically competing vegetation\u0000types that resemble grasslands and trees (the latter in the double stages of\u0000life: adults and seedlings). The newly developed model was applied to estimate\u0000how the climate-vegetation system reaches equilibrium across different rocky\u0000planetary configurations, and to assess its impact on temperature and\u0000habitability. With respect to a world with bare granite continents, the effect\u0000of vegetation-albedo feedback is to increase the average surface temperature.\u0000Since grasses and trees exhibit different albedos, they affect temperature to\u0000different degrees. The ultimate impact on climate depends on the outcome of the\u0000competition between these vegetation types. The change in albedo due to\u0000vegetation extends the habitable zone and enhances the overall planetary\u0000habitability beyond its traditional outer edge. This effect is especially\u0000relevant for planets that have a larger extension of continents than Earth. For\u0000Earth, the semi-major axis d = 1.04 UA represents the turning point where\u0000vegetation enhances habitability from h = 0.0 to h = 0.485 (in the\u0000grass-dominance case), to h = 0.584 (in the case of coexistence between grasses\u0000and trees), and to h = 0.612 (in the tree-dominance case). This illustrates the\u0000transition from a snowball state to a planet with intermediate habitability at\u0000the outer edge of the circumstellar habitability zone.","PeriodicalId":501209,"journal":{"name":"arXiv - PHYS - Earth and Planetary Astrophysics","volume":"4 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142204623","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}

{"title":"The GAPS programme at TNG LX Atmospheric characterisation of KELT-9 b via single-line analysis: Detection of six H I Balmer lines, Na I, Ca I, Ca II, Fe I, Fe II, Mg I, Ti II, Sc II, and Cr II","authors":"M. C. D'Arpa, A. Saba, F. Borsa, L. Fossati, G. Micela, C. Di Maio, M. Stangret, G. Tripodo, L. Affer, A. S. Bonomo, S. Benatti, M. Brogi, V. Fardella, A. F. Lanza, G. Guilluy, J. Maldonado, G. Mantovan, V. Nascimbeni, L. Pino, G. Scandariato, D. Sicilia, A. Sozzetti, R. Spinelli, G. Andreuzzi, A. Bignamini, R. Claudi, S. Desidera, A. Ghedina, C. Knapic, V. Lorenzi","doi":"arxiv-2409.01779","DOIUrl":"https://doi.org/arxiv-2409.01779","url":null,"abstract":"We analysed six primary transits of the ultra-hot Jupiter KELT-9,b obtained\u0000with the HARPS-N high-resolution spectrograph in the context of the Global\u0000Architecture of Planetary Systems (GAPS2) project, to characterise the\u0000atmosphere via single-line analysis. We extracted the transmission spectrum of\u0000each individual line by comparing the master out-of-transit spectrum with the\u0000in-transit spectra and computing the weighted average of the tomography in the\u0000planet reference frame. We corrected for the centre-to-limb variation and the\u0000Rossiter-McLaughlin effect by modelling the region of the star disc obscured by\u0000the planet during the transit and subtracting it from the master-out spectrum.\u0000We detected all six observable lines of the Balmer series within the HARPS-N\u0000wavelength range, from H$alpha$ to H$zeta$, with a significance exceeding\u00005$sigma$. We focussed on metal species, detecting Na I, Ca I, Ca II, Fe I, Fe\u0000II, Mg I, Ti II, Sc II, and Cr II lines. This is the first detection in the\u0000atmosphere of an exoplanet of H$epsilon$ and H$zeta$ lines, as well as of\u0000individual lines of Sc II and Cr II. Our detections are supported by a\u0000comparison with published synthetic transmission spectra of KELT-9b obtained\u0000accounting for non-local thermodynamic equilibrium effects. The results\u0000underline the presence of a systematic blueshift due to night-side to day-side\u0000winds. The single-line analysis allowed us not only to assess the presence of\u0000atomic species in the atmosphere of KELT-9 b, but also to further characterise\u0000the local stratification of the atmosphere. Coupling the height distribution of\u0000the detected species with the velocity shift retrieved, we acknowledged the\u0000height distribution of night-side to day-side winds. Moreover, the study of the\u0000rotational broadening of different species supports the prediction of a tidally\u0000locked planet rotating as a rigid body.","PeriodicalId":501209,"journal":{"name":"arXiv - PHYS - Earth and Planetary Astrophysics","volume":"42 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142204622","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}

{"title":"Hazardous Asteroids Classification","authors":"Thai Duy Quy, Alvin Buana, Josh Lee, Rakha Asyrofi","doi":"arxiv-2409.02150","DOIUrl":"https://doi.org/arxiv-2409.02150","url":null,"abstract":"Hazardous asteroid has been one of the concerns for humankind as fallen\u0000asteroid on earth could cost a huge impact on the society.Monitoring these\u0000objects could help predict future impact events, but such efforts are hindered\u0000by the large numbers of objects that pass in the Earth's vicinity. The aim of\u0000this project is to use machine learning and deep learning to accurately\u0000classify hazardous asteroids. A total of ten methods which consist of five\u0000machine learning algorithms and five deep learning models are trained and\u0000evaluated to find the suitable model that solves the issue. We experiment on\u0000two datasets, one from Kaggle and one we extracted from a web service called\u0000NeoWS which is a RESTful web service from NASA that provides information about\u0000near earth asteroids, it updates every day. In overall, the model is tested on\u0000two datasets with different features to find the most accurate model to perform\u0000the classification.","PeriodicalId":501209,"journal":{"name":"arXiv - PHYS - Earth and Planetary Astrophysics","volume":"9 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142204620","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}

{"title":"Storms and convection on Uranus and Neptune: impact of methane abundance revealed by a 3D cloud-resolving model","authors":"Noé Clément, Jérémy Leconte, Aymeric Spiga, Sandrine Guerlet, Franck Selsis, Gwenaël Milcareck, Lucas Teinturier, Thibault Cavalié, Raphaël Moreno, Emmanuel Lellouch, Óscar Carrión-González","doi":"arxiv-2409.02091","DOIUrl":"https://doi.org/arxiv-2409.02091","url":null,"abstract":"Uranus and Neptune have atmospheres dominated by molecular hydrogen and\u0000helium. In the upper troposphere, methane is the third main molecule and\u0000condenses, yielding a vertical gradient in CH4. This condensable species being\u0000heavier than H2 and He, the resulting change in mean molecular weight due to\u0000condensation comes as a factor countering dry and moist convection. As\u0000observations also show latitudinal variations in methane abundance, one can\u0000expect different vertical gradients from one latitude to another. In this\u0000paper, we investigate the impact of this methane vertical gradient on the\u0000atmospheric regimes, especially on the formation and inhibition of moist\u0000convective storms in the troposphere of ice giants. We develop a 3D\u0000cloud-resolving model to simulate convective processes. Using our simulations,\u0000we conclude that typical velocities of dry convection in the deep atmosphere\u0000are rather low (of the order of 1 m/s) but sufficient to sustain upward methane\u0000transport, and that moist convection at methane condensation level is strongly\u0000inhibited. Previous studies derived an analytical criterion on the methane\u0000vapor amount above which moist convection should be inhibited. We first\u0000validate this analytical criterion numerically. We then show that the critical\u0000methane abundance governs the inhibition and formation of moist convective\u0000storms, and we conclude that the intensity and intermittency of these storms\u0000should depend on the methane abundance and saturation. In ice giants, dry\u0000convection is weak, and moist convection is strongly inhibited. However, when\u0000enough methane is transported upwards, through dry convection and turbulent\u0000diffusion, sporadic moist convective storms can form. These storms should be\u0000more frequent on Neptune than on Uranus, because of Neptune's internal heat\u0000flow. Our results can explain the observed sporadicity of clouds in ice giants.","PeriodicalId":501209,"journal":{"name":"arXiv - PHYS - Earth and Planetary Astrophysics","volume":"1 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142204621","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}

{"title":"On-chain Validation of Tracking Data Messages (TDM) Using Distributed Deep Learning on a Proof of Stake (PoS) Blockchain","authors":"Yasir Latif, Anirban Chowdhury, Samya Bagchi","doi":"arxiv-2409.01614","DOIUrl":"https://doi.org/arxiv-2409.01614","url":null,"abstract":"Trustless tracking of Resident Space Objects (RSOs) is crucial for Space\u0000Situational Awareness (SSA), especially during adverse situations. The\u0000importance of transparent SSA cannot be overstated, as it is vital for ensuring\u0000space safety and security. In an era where RSO location information can be\u0000easily manipulated, the risk of RSOs being used as weapons is a growing\u0000concern. The Tracking Data Message (TDM) is a standardized format for\u0000broadcasting RSO observations. However, the varying quality of observations\u0000from diverse sensors poses challenges to SSA reliability. While many countries\u0000operate space assets, relatively few have SSA capabilities, making it crucial\u0000to ensure the accuracy and reliability of the data. Current practices assume\u0000complete trust in the transmitting party, leaving SSA capabilities vulnerable\u0000to adversarial actions such as spoofing TDMs. This work introduces a trustless\u0000mechanism for TDM validation and verification using deep learning over\u0000blockchain. By leveraging the trustless nature of blockchain, our approach\u0000eliminates the need for a central authority, establishing consensus-based\u0000truth. We propose a state-of-the-art, transformer-based orbit propagator that\u0000outperforms traditional methods like SGP4, enabling cross-validation of\u0000multiple observations for a single RSO. This deep learning-based transformer\u0000model can be distributed over a blockchain, allowing interested parties to host\u0000a node that contains a part of the distributed deep learning model. Our system\u0000comprises decentralised observers and validators within a Proof of Stake (PoS)\u0000blockchain. Observers contribute TDM data along with a stake to ensure honesty,\u0000while validators run the propagation and validation algorithms. The system\u0000rewards observers for contributing verified TDMs and penalizes those submitting\u0000unverifiable data.","PeriodicalId":501209,"journal":{"name":"arXiv - PHYS - Earth and Planetary Astrophysics","volume":"29 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142204630","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}

{"title":"TOI-2379 b and TOI-2384 b: two super-Jupiter mass planets transiting low-mass host stars","authors":"Edward M. Bryant, Daniel Bayliss, Joel D. Hartman, Elyar Sedaghati, Melissa J. Hobson, Andrés Jordán, Rafael Brahm, Gaspar Á. Bakos, Jose Manuel Almenara, Khalid Barkaoui, Xavier Bonfils, Marion Cointepas, Karen A. Collins, Georgina Dransfield, Phil Evans, Michaël Gillon, Emmanuël Jehin, Felipe Murgas, Francisco J. Pozuelos, Richard P. Schwarz, Mathilde Timmermans, Cristilyn N. Watkins, Anaël Wünsche, R. Paul Butler, Jeffrey D. Crane, Steve Shectman, Johanna K. Teske, David Charbonneau, Zahra Essack, Jon M. Jenkins, Hannah M. Lewis, Sara Seager, Eric B. Ting, Joshua N. Winn","doi":"arxiv-2409.01239","DOIUrl":"https://doi.org/arxiv-2409.01239","url":null,"abstract":"Short-period gas giant planets have been shown to be significantly rarer for\u0000host stars less massive than the Sun. We report the discovery of two transiting\u0000giant planets - TOI-2379 b and TOI-2384 b - with low-mass (early M) host stars.\u0000Both planets were detected using TESS photometry and for both the transit\u0000signal was validated using ground based photometric facilities. We confirm the\u0000planetary nature of these companions and measure their masses using radial\u0000velocity observations. We find that TOI-2379 b has an orbital period of 5.469 d\u0000and a mass and radius of $5.76pm0.20$ M$_{J}$ and $1.046pm0.023$ R$_{J}$ and\u0000TOI-2384 b has an orbital period of 2.136 d and a mass and radius of\u0000$1.966pm0.059$ M$_{J}$ and $1.025pm0.021$ R$_{J}$. TOI-2379 b and TOI-2384 b\u0000have the highest and third highest planet-to-star mass ratios respectively out\u0000of all transiting exoplanets with a low-mass host star, placing them uniquely\u0000among the population of known exoplanets and making them highly important\u0000pieces of the puzzle for understanding the extremes of giant planet formation.","PeriodicalId":501209,"journal":{"name":"arXiv - PHYS - Earth and Planetary Astrophysics","volume":"22 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142204624","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}

{"title":"RedDots: Limits on habitable and undetected planets orbiting nearby stars GJ 832, GJ 674, and Ross 128","authors":"F. Liebing, S. V. Jeffers, P. Gorrini, C. A. Haswell, S. Dreizler, J. R. Barnes, C. Hartogh, V. Koseleva, F. Del Sordo, P. J. Amado, J. A. Caballero, M. J. López-González, N. Morales, A. Reiners, I. Ribas, A. Quirrenbach, E. Rodríguez, L. Tal-Or, Y. Tsapras","doi":"arxiv-2409.01173","DOIUrl":"https://doi.org/arxiv-2409.01173","url":null,"abstract":"Aims. Using HARPS spectroscopic data obtained by the RedDots campaign, as\u0000well as archival data from HARPS and CARMENES, supplemented with ASH2 and T90\u0000photometry, we aim to search for additional planets around the three M dwarfs\u0000GJ 832, GJ 674, and Ross 128. We also aim to determine limits on possible\u0000undetected, habitable planets. We investigate (i) the reliability of the\u0000recovered orbital eccentricities and (ii) the reliability of Bayesian evidence\u0000as a diagnostic for selecting the best model. Methods. We employed Markov-chain Monte Carlo, nested sampling, and Gaussian\u0000process (GP) analyses to fit a total of 20 different models. We used the\u0000residuals to create grids for injection-recovery simulations to obtain\u0000detection limits on potentially undiscovered planets. Results. Our refined orbital elements for GJ 832 b, GJ 674 b, and Ross 128 b\u0000confirm (GJ 832, GJ 674) or increase (Ross 128) prior eccentricity\u0000determinations. No additional planets were found in any of the systems. The\u0000detection limits obtained for all three systems are between 30 and 50 cm/s for\u0000orbital periods in the range of 1 to 10 000 days. Using N-body simulations, we\u0000find that undiscovered secondary planets are unlikely (Ross 128) or incapable\u0000(GJ 674) of having caused the observed eccentricities of the known planets. We\u0000find that the eccentricity of GJ 832 b is not significantly different from\u0000zero. Conclusions. GJ 832 b, GJ 674 b, and Ross 128 b retain their status as\u0000hosting lonely and (for the latter two) eccentric planets. Finally, our results\u0000show that Bayesian evidence, when used in conjunction with GP, is not a robust\u0000diagnostic for selecting the best model in cases of low-activity stars. In such\u0000cases, we advise an inspection of the shapes of the posterior distributions and\u0000to ensure that relevant simulations are performed to assess the validity of the\u0000perceived best model.","PeriodicalId":501209,"journal":{"name":"arXiv - PHYS - Earth and Planetary Astrophysics","volume":"19 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142204626","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}

{"title":"Twin Worlds, Divergent Fates: How Obliquity has differently shaped Pluto's and Triton's landscapes and climates","authors":"Tanguy Bertrand, François Forget, Emmanuel Lellouch","doi":"arxiv-2409.01122","DOIUrl":"https://doi.org/arxiv-2409.01122","url":null,"abstract":"Triton and Pluto are believed to share a common origin, both forming\u0000initially in the Kuiper Belt but Triton being later captured by Neptune. Both\u0000objects display similar sizes, densities, and atmospheric and surface ice\u0000composition, with the presence of volatile ices N2, CH4 and CO. Yet their\u0000appearance, including their surface albedo and ice distribution strongly\u0000differ. What can explain these different appearances? A first disparity is that\u0000Triton is experiencing significant tidal heating due to its orbit around\u0000Neptune, with subsequent resurfacing and a relatively flat surface, while Pluto\u0000is not tidally activated and displays a pronounced topography. Here we present\u0000long-term volatile transport simulations of Pluto and Triton, using the same\u0000initial conditions and volatile inventory, but with the known orbit and\u0000rotation of each object. The model reproduces, to first order, the observed\u0000volatile ice surface distribution on Pluto and Triton. Our results\u0000unambiguously demonstrate that obliquity is the main driver of the differences\u0000in surface appearance and in climate properties on Pluto and Triton, and give\u0000further support to the hypothesis that both objects had a common origin\u0000followed by a different dynamical history.","PeriodicalId":501209,"journal":{"name":"arXiv - PHYS - Earth and Planetary Astrophysics","volume":"50 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142204627","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}

{"title":"Searching for GEMS: TOI-5688 A b, a low-density giant orbiting a high-metallicity early M-dwarf","authors":"Varghese Reji, Shubham Kanodia, Joe Ninan, Caleb I. Cañas, Jessica Libby-Roberts, Andrea S. J. Lin, Arvind F Gupta, Tera N. Sewaby, Alexander Larsen, Henry A. Kobulnicky, Philip I. Choi, Nez Evans, Sage Santomenna, Isabelle Winnick, Larry Yu, Jaime A. Alvarado-Montes, Chad Bender, Lia Marta Bernabò, Cullen H. Blake, William D. Cochran, Scott A. Diddams, Samuel Halverson, Te Han, Fred Hearty, Sarah E. Logsdon, Suvrath Mahadevan, Andrew Monson, Michael McElwain, Paul Robertson, Devendra Ojha, Arpita Roy, Christian Schwab, Gudmundur Stefansson, Jason Wright","doi":"arxiv-2409.01371","DOIUrl":"https://doi.org/arxiv-2409.01371","url":null,"abstract":"We present the discovery of a low-density planet transiting TOI-5688 A b, a\u0000high-metallicity M2V star. This planet was discovered as part of the search for\u0000transiting giant planets ($R gtrsim8$ M$_oplus$) through the Searching for\u0000GEMS (Giant Exoplanets around M-dwarf Stars) survey. The planet TOI-5688 A b\u0000was discovered with the Transiting Exoplanet Survey Satellite (TESS), and\u0000characterized with ground-based transits from Red Buttes Observatory (RBO), the\u0000Table Mountain Observatory of Pomona College, and radial velocity (RV)\u0000measurements with the Habitable-Zone Planet Finder (HPF) on the 10 m Hobby\u0000Eberly Telescope (HET) and NEID on the WIYN 3.5 m telescope. From the joint fit\u0000of transit and RV data, the mass of the planet is $124pm24$ M$_oplus$ and the\u0000radius is $10.4pm0.7$ R$_oplus$. This planet has a density of\u0000$0.61^{+0.20}_{-0.15}$ g/cm${}^3$, and is on a $sim2.95$ day orbit around its\u0000host star. The spectroscopic and photometric analysis of the host star TOI-5688\u0000A shows that it is a high metallicity ([Fe/H] $ = 0.47pm0.16$ dex) M2V star,\u0000favoring the core-accretion formation pathway as the likely formation scenario\u0000for this planet. In this paper, we analyze potential mechanisms of planet\u0000formation in the context of the formation of TOI-5688 A b. Additionally,\u0000observations with Gaia suggest the presence of a wide-separation binary\u0000companion, TOI-5688 B, which has a projected separation of $sim5\"$ (1110 AU)\u0000and is an M4V. This makes TOI-5688 A b part of a growing number of GEMS in\u0000wide-separation binary systems.","PeriodicalId":501209,"journal":{"name":"arXiv - PHYS - Earth and Planetary Astrophysics","volume":"18 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142204625","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}

{"title":"Misaligned Disk and Stellar Oblateness Driven Sculpting of Exoplanetary Systems: Origin of Perpendicular Orbits in HD 3167","authors":"Tao Fu, Yue Wang","doi":"arxiv-2409.00506","DOIUrl":"https://doi.org/arxiv-2409.00506","url":null,"abstract":"A significant proportion of exoplanets have been detected with highly tilted\u0000or even polar orbits relative to their host stars' equatorial planes. These\u0000unusual orbital configurations are often linked to post-disk secular\u0000interactions among multiple bodies. However, many aspects remain elusive. In\u0000this study, we investigate the role of disk-induced spin-orbit misalignments in\u0000shaping architecture of multi-planet systems, taking into account the combined\u0000effect of the host star's oblateness and the full-space disk potential. We\u0000demonstrate that large mutual planetary inclinations can arise from a\u0000saddle-center bifurcation occurring during the photoevaporation of the disk.\u0000This bifurcation triggers an instant, non-adiabatic transition in the planet's\u0000libration. Following this process, the orbital evolution diverges into several\u0000distinct patterns. Notably, in scenarios involving a near-polar primordial\u0000misalignment, the orbit, consistently librating about a coplanar equilibrium\u0000axis, can be captured by an orthogonal equilibrium during the decay of the\u0000stellar oblateness. However, the orbit will be eventually recaptured by the\u0000coplanar equilibrium, aligned or anti-aligned with the orientation of the outer\u0000orbit, resulting in either a prograde or retrograde inner-outer orbit\u0000configuration. Additionally, general relativity contributes to maintaining\u0000eccentricity stability within these dynamic scenarios. Through the proposed\u0000mechanism, we can provide a plausible explanation for the unique,\u0000near-perpendicular and likely retrograde orbit architecture observed in the HD\u00003167 system, enhancing our understanding of exoplanetary system dynamics.","PeriodicalId":501209,"journal":{"name":"arXiv - PHYS - Earth and Planetary Astrophysics","volume":"23 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-08-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142204628","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}