Pub Date : 2018-12-03DOI: 10.2458/azu_uapress_9780816540068
S. Raymond, A. Izidoro, A. Morbidelli
Exoplanet surveys have confirmed one of humanity's (and all teenagers') worst fears: we are weird. If our Solar System were observed with present-day Earth technology -- to put our system and exoplanets on the same footing -- Jupiter is the only planet that would be detectable. The statistics of exo-Jupiters indicate that the Solar System is unusual at the ~1% level among Sun-like stars (or ~0.1% among all stars). But why are we different? Successful formation models for both the Solar System and exoplanet systems rely on two key processes: orbital migration and dynamical instability. Systems of close-in super-Earths or sub-Neptunes require substantial radial inward motion of solids either as drifting mm- to cm-sized pebbles or migrating Earth-mass or larger planetary embryos. We argue that, regardless of their formation mode, the late evolution of super-Earth systems involves migration into chains of mean motion resonances, generally followed by instability when the disk dissipates. This pattern is likely also ubiquitous in giant planet systems. We present three models for inner Solar System formation -- the low-mass asteroid belt, Grand Tack, and Early Instability models -- each invoking a combination of migration and instability. We identify bifurcation points in planetary system formation. We present a series of events to explain why our Solar System is so weird. Jupiter's core must have formed fast enough to quench the growth of Earth's building blocks by blocking the flux of inward-drifting pebbles. The large Jupiter/Saturn mass ratio is rare among giant exoplanets but may be required to maintain Jupiter's wide orbit. The giant planets' instability must have been gentle, with no close encounters between Jupiter and Saturn, also unusual in the larger (exoplanet) context. Our Solar System system is thus the outcome of multiple unusual, but not unheard of, events.
{"title":"Solar System Formation in the Context of Extra-Solar Planets","authors":"S. Raymond, A. Izidoro, A. Morbidelli","doi":"10.2458/azu_uapress_9780816540068","DOIUrl":"https://doi.org/10.2458/azu_uapress_9780816540068","url":null,"abstract":"Exoplanet surveys have confirmed one of humanity's (and all teenagers') worst fears: we are weird. If our Solar System were observed with present-day Earth technology -- to put our system and exoplanets on the same footing -- Jupiter is the only planet that would be detectable. The statistics of exo-Jupiters indicate that the Solar System is unusual at the ~1% level among Sun-like stars (or ~0.1% among all stars). But why are we different? Successful formation models for both the Solar System and exoplanet systems rely on two key processes: orbital migration and dynamical instability. Systems of close-in super-Earths or sub-Neptunes require substantial radial inward motion of solids either as drifting mm- to cm-sized pebbles or migrating Earth-mass or larger planetary embryos. We argue that, regardless of their formation mode, the late evolution of super-Earth systems involves migration into chains of mean motion resonances, generally followed by instability when the disk dissipates. This pattern is likely also ubiquitous in giant planet systems. We present three models for inner Solar System formation -- the low-mass asteroid belt, Grand Tack, and Early Instability models -- each invoking a combination of migration and instability. We identify bifurcation points in planetary system formation. We present a series of events to explain why our Solar System is so weird. Jupiter's core must have formed fast enough to quench the growth of Earth's building blocks by blocking the flux of inward-drifting pebbles. The large Jupiter/Saturn mass ratio is rare among giant exoplanets but may be required to maintain Jupiter's wide orbit. The giant planets' instability must have been gentle, with no close encounters between Jupiter and Saturn, also unusual in the larger (exoplanet) context. Our Solar System system is thus the outcome of multiple unusual, but not unheard of, events.","PeriodicalId":8428,"journal":{"name":"arXiv: Earth and Planetary Astrophysics","volume":"11 2 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2018-12-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"78411410","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}
Pub Date : 2018-12-01DOI: 10.32023/0001-5237/68.4.4
G. Maciejewski, M. Fern'andez, F. Aceituno, S. Mart'in-Ruiz, J. Ohlert, D. Dimitrov, K. Szyszka, C. V. Essen, M. Mugrauer, R. Bischoff, K. Michel, M. Mallonn, M. Stangret, D. Mo'zdzierski
Theoretical calculations and some indirect observations show that massive exoplanets on tight orbits must decay due to tidal dissipation within their host stars. This orbital evolution could be observationally accessible through precise transit timing over a course of decades. The rate of planetary in-spiralling may not only help us to understand some aspects of evolution of planetary systems, but also can be used as a probe of the stellar internal structure. In this paper we present results of transit timing campaigns organised for a carefully selected sample of hot Jupiter-like planets which were found to be the best candidates for detecting planet-star tidal interactions on the Northern hemisphere. Among them, there is the WASP-12 system which is the best candidate for possessing an in-falling giant exoplanet. Our new observations support the scenario of orbital decay of WASP-12 b and allow us to refine its rate. The derived tidal quality parameter of the host star Q'_{*} = (1.82 +/- 0.32) x 10^5 is in agreement with theoretical predictions for subgiant stars. For the remaining systems - HAT-P-23, KELT-1, KELT-16, WASP-33, and WASP-103 - our transit timing data reveal no deviations from the constant-period models, hence constraints on the individual rates of orbital decay were placed. The tidal quality parameters of host stars in at least 4 systems - HAT-P-23, KELT-1, WASP-33, and WASP-103 - were found to be greater than the value reported for WASP-12. This is in line with the finding that those hosts are main sequence stars, for which efficiency of tidal dissipation is predicted to be relatively weak.
{"title":"Planet-star interactions with precise transit timing. I. The refined orbital decay rate for WASP-12 b and initial constraints for HAT-P-23 b, KELT-1 b, KELT-16 b, WASP-33 b, and WASP-103 b","authors":"G. Maciejewski, M. Fern'andez, F. Aceituno, S. Mart'in-Ruiz, J. Ohlert, D. Dimitrov, K. Szyszka, C. V. Essen, M. Mugrauer, R. Bischoff, K. Michel, M. Mallonn, M. Stangret, D. Mo'zdzierski","doi":"10.32023/0001-5237/68.4.4","DOIUrl":"https://doi.org/10.32023/0001-5237/68.4.4","url":null,"abstract":"Theoretical calculations and some indirect observations show that massive exoplanets on tight orbits must decay due to tidal dissipation within their host stars. This orbital evolution could be observationally accessible through precise transit timing over a course of decades. The rate of planetary in-spiralling may not only help us to understand some aspects of evolution of planetary systems, but also can be used as a probe of the stellar internal structure. In this paper we present results of transit timing campaigns organised for a carefully selected sample of hot Jupiter-like planets which were found to be the best candidates for detecting planet-star tidal interactions on the Northern hemisphere. Among them, there is the WASP-12 system which is the best candidate for possessing an in-falling giant exoplanet. Our new observations support the scenario of orbital decay of WASP-12 b and allow us to refine its rate. The derived tidal quality parameter of the host star Q'_{*} = (1.82 +/- 0.32) x 10^5 is in agreement with theoretical predictions for subgiant stars. For the remaining systems - HAT-P-23, KELT-1, KELT-16, WASP-33, and WASP-103 - our transit timing data reveal no deviations from the constant-period models, hence constraints on the individual rates of orbital decay were placed. The tidal quality parameters of host stars in at least 4 systems - HAT-P-23, KELT-1, WASP-33, and WASP-103 - were found to be greater than the value reported for WASP-12. This is in line with the finding that those hosts are main sequence stars, for which efficiency of tidal dissipation is predicted to be relatively weak.","PeriodicalId":8428,"journal":{"name":"arXiv: Earth and Planetary Astrophysics","volume":"8 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2018-12-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"81798882","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}
Pub Date : 2018-10-13DOI: 10.1017/9781316339794.002
E. Asphaug
Terrestrial planets grew in a series of similar-sized collisions that swept up most of the next-largest bodies. Theia was accreted by the Earth to form the Moon according to the theory. Planetesimals likewise may have finished their accretion in a sequence of 'junior giant impacts', scaled down in size and velocity. This chapter considers the complicated physics of pairwise accretion, as planetesimals grow to planetary scales, and considers how the inefficiency of that process influences the origin of planetesimals and the diversity of meteorites and primary asteroids.
{"title":"Signatures of Hit-and-run Collisions","authors":"E. Asphaug","doi":"10.1017/9781316339794.002","DOIUrl":"https://doi.org/10.1017/9781316339794.002","url":null,"abstract":"Terrestrial planets grew in a series of similar-sized collisions that swept up most of the next-largest bodies. Theia was accreted by the Earth to form the Moon according to the theory. Planetesimals likewise may have finished their accretion in a sequence of 'junior giant impacts', scaled down in size and velocity. This chapter considers the complicated physics of pairwise accretion, as planetesimals grow to planetary scales, and considers how the inefficiency of that process influences the origin of planetesimals and the diversity of meteorites and primary asteroids.","PeriodicalId":8428,"journal":{"name":"arXiv: Earth and Planetary Astrophysics","volume":"47 1","pages":"7-37"},"PeriodicalIF":0.0,"publicationDate":"2018-10-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"76733480","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}
H. Campins, J. Leon, J. Licandro, A. Hendrix, Juan A. Sanchez, V. Alí-Lagoa
{"title":"Compositional Diversity Among Primitive Asteroids","authors":"H. Campins, J. Leon, J. Licandro, A. Hendrix, Juan A. Sanchez, V. Alí-Lagoa","doi":"10.1016/C2016-0-05001-5","DOIUrl":"https://doi.org/10.1016/C2016-0-05001-5","url":null,"abstract":"","PeriodicalId":8428,"journal":{"name":"arXiv: Earth and Planetary Astrophysics","volume":"29 1","pages":"345-369"},"PeriodicalIF":0.0,"publicationDate":"2018-09-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"74047688","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}
E. Carolo, D. Vassallo, J. Farinato, G. Agapito, M. Bergomi, A. Carlotti, M. D. Pascale, V. D’Orazi, D. Greggio, D. Magrin, L. Marafatto, D. Mesa, E. Pinna, A. Puglisi, M. Stangalini, C. Vérinaud, V. Viotto, F. Biondi, S. Chinellato, M. Dima, S. Esposito, F. Pedichini, E. Portaluri, R. Ragazzoni, G. Umbriaco
A robust post processing technique is mandatory to analyse the coronagraphic high contrast imaging data. Angular Differential Imaging (ADI) and Principal Component Analysis (PCA) are the most used approaches to suppress the quasi-static structure in the Point Spread Function (PSF) in order to revealing planets at different separations from the host star. The focus of this work is to apply these two data reduction techniques to obtain the best limit detection for each coronagraphic setting that has been simulated for the SHARK-NIR, a coronagraphic camera that will be implemented at the Large Binocular Telescope (LBT). We investigated different seeing conditions ($0.4"-1"$) for stellar magnitude ranging from R=6 to R=14, with particular care in finding the best compromise between quasi-static speckle subtraction and planet detection.
{"title":"Data processing on simulated data for SHARK-NIR.","authors":"E. Carolo, D. Vassallo, J. Farinato, G. Agapito, M. Bergomi, A. Carlotti, M. D. Pascale, V. D’Orazi, D. Greggio, D. Magrin, L. Marafatto, D. Mesa, E. Pinna, A. Puglisi, M. Stangalini, C. Vérinaud, V. Viotto, F. Biondi, S. Chinellato, M. Dima, S. Esposito, F. Pedichini, E. Portaluri, R. Ragazzoni, G. Umbriaco","doi":"10.26698/AO4ELT5.0068","DOIUrl":"https://doi.org/10.26698/AO4ELT5.0068","url":null,"abstract":"A robust post processing technique is mandatory to analyse the coronagraphic high contrast imaging data. Angular Differential Imaging (ADI) and Principal Component Analysis (PCA) are the most used approaches to suppress the quasi-static structure in the Point Spread Function (PSF) in order to revealing planets at different separations from the host star. The focus of this work is to apply these two data reduction techniques to obtain the best limit detection for each coronagraphic setting that has been simulated for the SHARK-NIR, a coronagraphic camera that will be implemented at the Large Binocular Telescope (LBT). We investigated different seeing conditions ($0.4\"-1\"$) for stellar magnitude ranging from R=6 to R=14, with particular care in finding the best compromise between quasi-static speckle subtraction and planet detection.","PeriodicalId":8428,"journal":{"name":"arXiv: Earth and Planetary Astrophysics","volume":"14 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2018-08-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"78249412","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}
Pub Date : 2018-07-25DOI: 10.1007/978-3-319-55333-7_137
E. Bergin, L. Cleeves
{"title":"Chemistry During the Gas-rich Stage of Planet Formation","authors":"E. Bergin, L. Cleeves","doi":"10.1007/978-3-319-55333-7_137","DOIUrl":"https://doi.org/10.1007/978-3-319-55333-7_137","url":null,"abstract":"","PeriodicalId":8428,"journal":{"name":"arXiv: Earth and Planetary Astrophysics","volume":"16 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2018-07-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"73160482","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}
Pub Date : 2018-07-16DOI: 10.32023/0001-5237/69.2.3
Alexis M. S. Smith, S. Csizmadia, D. Gandolfi, S. Albrecht, R. Alonso, O. Barragán, J. Cabrera, W. Cochran, F. Dai, H. Deeg, P. Eigmüller, M. Endl, A. Erikson, M. Fridlund, Akihiko Fukui, S. Grziwa, E. Guenther, A. Hatzes, D. Hidalgo, T. Hirano, J. Korth, M. Kuzuhara, J. Livingston, N. Narita, D. Nespral, P. Niraula, G. Nowak, E. Pallé, M. Pätzold, C. M. Persson, J. Prieto-Arranz, H. Rauer, Seth Redfield, Ignasi Ribas, V. V. Eylen
We report the discovery from K2 of two transiting hot Jupiter systems. EPIC 220501947 (observed in Campaign 8) is a K5 dwarf which hosts a planet slightly smaller than Jupiter, orbiting with a period of 4.0 d. We have made an independent discovery of K2-237 b (Campaign 11), which orbits an F6 dwarf every 2.2 d and has an inflated radius 50 - 60 per cent larger than that of Jupiter. We use high-precision radial velocity measurements, obtained using the HARPS and FIES spectrographs, to measure the planetary masses. We find that EPIC 220501947 b has a similar mass to Saturn, while K2-237 b is a little more massive than Jupiter.
{"title":"EPIC 220501947 b and K2-237 b: two transiting hot Jupiters","authors":"Alexis M. S. Smith, S. Csizmadia, D. Gandolfi, S. Albrecht, R. Alonso, O. Barragán, J. Cabrera, W. Cochran, F. Dai, H. Deeg, P. Eigmüller, M. Endl, A. Erikson, M. Fridlund, Akihiko Fukui, S. Grziwa, E. Guenther, A. Hatzes, D. Hidalgo, T. Hirano, J. Korth, M. Kuzuhara, J. Livingston, N. Narita, D. Nespral, P. Niraula, G. Nowak, E. Pallé, M. Pätzold, C. M. Persson, J. Prieto-Arranz, H. Rauer, Seth Redfield, Ignasi Ribas, V. V. Eylen","doi":"10.32023/0001-5237/69.2.3","DOIUrl":"https://doi.org/10.32023/0001-5237/69.2.3","url":null,"abstract":"We report the discovery from K2 of two transiting hot Jupiter systems. EPIC 220501947 (observed in Campaign 8) is a K5 dwarf which hosts a planet slightly smaller than Jupiter, orbiting with a period of 4.0 d. We have made an independent discovery of K2-237 b (Campaign 11), which orbits an F6 dwarf every 2.2 d and has an inflated radius 50 - 60 per cent larger than that of Jupiter. We use high-precision radial velocity measurements, obtained using the HARPS and FIES spectrographs, to measure the planetary masses. We find that EPIC 220501947 b has a similar mass to Saturn, while K2-237 b is a little more massive than Jupiter.","PeriodicalId":8428,"journal":{"name":"arXiv: Earth and Planetary Astrophysics","volume":"29 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2018-07-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"73124997","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}
Pub Date : 2018-07-13DOI: 10.1007/978-3-319-55333-7_101
B. Biller, M. Bonnefoy
{"title":"Exoplanet Atmosphere Measurements from Direct Imaging","authors":"B. Biller, M. Bonnefoy","doi":"10.1007/978-3-319-55333-7_101","DOIUrl":"https://doi.org/10.1007/978-3-319-55333-7_101","url":null,"abstract":"","PeriodicalId":8428,"journal":{"name":"arXiv: Earth and Planetary Astrophysics","volume":"4 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2018-07-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"74476119","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}
Cabral Nahuel, N. Lagarde, C. Reyl'e, A. Guilbert-Lepoutre, A. Robin
Connecting star and planet properties in a single model is not straightforward. Stellar population synthesis models are key to explore combined statistical constraints from stars and planets observations. The Besancon stellar population synthesis model (Robin et al. 2003, Lagarde et al. 2017) includes now the stellar evolutionary tracks computed with the stellar evolution code STAREVOL (Lagarde et al. 2012, Amard et al. 2016). It provides the global (M, R, Teff, etc) and chemical properties of stars for 54 chemical species. It enables to study the different galactic populations of the Milky Way (the halo, the bulge, the thin and thick disc) and a specific observational survey. Here, we couple the Besancon model with a simple stoichiometric model (Santos et al. 2017) in order to determine the expected composition of the planet building blocks (PBB). We investigate the trends and correlations of the expected chemical abundances of PBB in the different stellar populations of the Milky Way (Cabral et al. 2018).
在单一模型中连接恒星和行星的属性并不简单。恒星人口综合模型是探索恒星和行星观测的联合统计约束的关键。Besancon恒星群综合模型(Robin et al. 2003, Lagarde et al. 2017)现在包括用恒星演化代码STAREVOL计算的恒星演化轨迹(Lagarde et al. 2012, Amard et al. 2016)。它提供了54种化学物质的全局(M, R, Teff等)和化学性质。它可以研究银河系的不同星系群(光环、凸起、薄盘和厚盘)，并进行具体的观测调查。在这里，我们将Besancon模型与一个简单的化学计量模型(Santos et al. 2017)结合起来，以确定行星构建块(PBB)的预期组成。我们研究了银河系不同恒星群中PBB预期化学丰度的趋势和相关性(Cabral et al. 2018)。
{"title":"Chemical connections between low-mass stars and planets building blocks investigated by stellar population synthesis","authors":"Cabral Nahuel, N. Lagarde, C. Reyl'e, A. Guilbert-Lepoutre, A. Robin","doi":"10.5281/ZENODO.1489206","DOIUrl":"https://doi.org/10.5281/ZENODO.1489206","url":null,"abstract":"Connecting star and planet properties in a single model is not straightforward. Stellar population synthesis models are key to explore combined statistical constraints from stars and planets observations. The Besancon stellar population synthesis model (Robin et al. 2003, Lagarde et al. 2017) includes now the stellar evolutionary tracks computed with the stellar evolution code STAREVOL (Lagarde et al. 2012, Amard et al. 2016). It provides the global (M, R, Teff, etc) and chemical properties of stars for 54 chemical species. It enables to study the different galactic populations of the Milky Way (the halo, the bulge, the thin and thick disc) and a specific observational survey. Here, we couple the Besancon model with a simple stoichiometric model (Santos et al. 2017) in order to determine the expected composition of the planet building blocks (PBB). We investigate the trends and correlations of the expected chemical abundances of PBB in the different stellar populations of the Milky Way (Cabral et al. 2018).","PeriodicalId":8428,"journal":{"name":"arXiv: Earth and Planetary Astrophysics","volume":"2 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2018-07-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"89757463","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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