Imaging the Key Stages of Planet Formation
John D. MonnierGioia RauJ. Sánchez-BermúdezSam RaglandRachel AkesonGaspard DuchêneGerald van BelleRyan NorrisKathryn GordonDenis DefrèreJ. KluskaStephen T. RidgwayJ.-B. Le BouquinNarsireddy AnuguNicholas J. ScottStephen KaneNoel D. RichardsonZsolt RegalyZhaohuan ZhuGautam VasishtKeivan G. StassunSean M. AndrewsS. LacourG. WeigeltN. TurnerFred C. AdamsDouglas R. GiesNuria CalvetCatherine EspaillatR. Millan‐GabetTyler GardnerC. PackhamM. GaiQuentin KralJean-Philippe BergerH. LinzLucia KlarmannMatthew R. BateJaehan BaeR. García LópezA. GarufiFabien BaronMihkel KamaDavid J. WilnerLee HartmannMakoto KishimotoJ. OlofssonMelissa McclureC. HaniffS. HoenigMichael R. LineR. G. PetrovMichael SmithTheo A. ten BrummelaarMatthew De FurioM. KoutoulakiStephen A. RinehartDavid LeisawitzW. C. DanchiDaniel HuberKe ZhangBenjamin PopeMichael IrelandStefan KrausAndrea IsellaBenjamin R. SetterholmR. J. White
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Abstract:
New images of young stars are revolutionizing our understanding of planet formation. ALMA detects large grains in planet-forming disks with few AU scale resolution and scattered light imaging with extreme adaptive optics systems reveal small grains suspended on the disks' flared surfaces. Tantalizing evidence for young exoplanets is emerging from line observations of CO and H-alpha. In this white paper, we explore how even higher angular resolution can extend our understanding of the key stages of planet formation, to resolve accreting circumplanetary disks themselves, and to watch planets forming in situ for the nearest star-forming regions. We focus on infrared observations which are sensitive to thermal emission in the terrestrial planet formation zone and allow access to molecular tracers in warm ro-vibrational states. Successful planet formation theories will not only be able to explain the diverse features seen in disks, but will also be consistent with the rich exoplanet demographics from RV and transit surveys. While we are far from exhausting ground-based techniques, the ultimate combination of high angular resolution and high infrared sensitivity can only be achieved through mid-infrared space interferometry.Keywords:
Dwarf planet
The colloquium "Detection and Dynamics of Transiting Exoplanets" was held at the Observatoire de Haute-Provence and discussed the status of transiting exoplanet investigations in a 4.5 day meeting. Topics addressed ranged from planet detection, a discussion on planet composition and interior structure, atmospheres of hot-Jupiter planets, up to the effect of tides and the dynamical evolution of planetary systems. Here, I give a summary of the recent developments of transiting planet detections and investigations discussed at this meeting.
Jupiter (rocket family)
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"An Introduction to Planets. Ours and Others; From Earth to Exoplanets, by Therese Encrenaz." Contemporary Physics, 56(4), p. 511
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A NEW CONCEPT FOR DIRECT IMAGING AND SPECTRAL CHARACTERIZATION OF EXOPLANETS IN MULTI-PLANET SYSTEMS
We present a novel method for direct detection and characterization of exoplanets from space. This method uses four collecting telescopes, combined with phase chopping and a spectrometer, with observations on only a few baselines rather than on a continuously rotated baseline. Focusing on the contiguous wavelength spectra of typical exoplanets, the (u, v) plane can be simultaneously and uniformly filled by recording the spectrally resolved signal. This concept allows us to perfectly remove speckles from reconstructed images. For a target comprising a star and multiple planets, observations on three baselines are sufficient to extract the position and spectrum of each planet. Our simulations show that this new method allows us to detect an analog Earth around a Sun-like star at 10 pc and to acquire its spectrum over the wavelength range from 8 to 19 {\mu}m with a high spectral resolution of 100. This method allows us to fully characterize an analog Earth and to similarly characterize each planet in multi-planet systems.
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Detecting exoplanets has become a hot topic, where various detection scenarios have been proposed. Five of these methods have all found more than 50 exoplanets, which are the transit method, the radial velocity method, the microlensing method, the imaging method, and the timing method. This paper aims to find their pros and cons, and the type of exoplanet that is suitable for each method by comparing the characteristics of exoplanets found by each method and the detection result of each method. The transit method is suitable for exoplanets with short periods possessing the advantages of measuring various parameters of exoplanets simultaneously, but can confuse exoplanets and other celestial bodies with the same radius of planets. The radial velocity method is best for exoplanets with small orbit radius or large mass, whereas it can only determine the minimum mass of exoplanets. The microlensing method can find exoplanets that are extremely far from the Earth or even rogue planets, as well as their mass. However, it does not allow researchers to observe the exoplanets found by it twice. The imaging method offers a tool to directly observe exoplanets in the infrared band. It can detect exoplanets that are extremely far from their host star with relatively high temperatures or rogue planets, but these are also the types of exoplanets that it can be detected. The timing method allows observers to discover exoplanets around pulsars, pulsating stars, eclipsing binaries, and planetary systems with discovered planets, but it is limited to these types.
Gravitational microlensing
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In this work, we present transit timing variations detected for the exoplanet TrES-5b. To obtain the necessary amount of photometric data for this exoplanet, we have organized an international campaign to search for exoplanets based on the Transit Timing Variation method (TTV) and as a result of this we collected 30 new light curves, 15 light curves from the Exoplanet Transit Database (ETD) and 8 light curves from the literature for the timing analysis of the exoplanet TrES-5b. We have detected timing variations with a semi-amplitude of A ~ 0.0016 days and a period of P ~ 99 days. We carried out the N-body modeling based on the three-body problem. The detected perturbation of TrES-5b may be caused by a second exoplanet in the TrES-5 system. We have calculated the possible mass and resonance of the object: M ~ 0.24MJup at a 1:2 Resonance.
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Planets are common around Sun-like stars. ‘Exoplanets’ examines this type of planet. The first discovery of an exoplanet was made in 1995, and hundreds of exoplanets are now known to exist. Exoplanets have been found by detecting slight changes in a star's radial velocity, and by looking for ‘transits’ (a tiny fraction of a star's light that is cut off during the passage of an exoplanet in front of it) using Earth-based and space-based automated telescopes. What do we actually know about exoplanets? Are they named? How do we image them? How many multiple exoplanet systems are there, and is it possible that life could thrive on exoplanets?
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Exoplanets are planets orbiting a star other than the Sun. These exoplanets may exist in many different forms, such as a hot Jupiter and super earth. Detecting is the first step to further studying the properties of these exoplanets. In this paper, based on data of star Qatar-1 gathered from July 22nd 2022, a light flux curve is developed during the period of 04:28 - 07:01 UTC through which the star is observed. The presence of an exoplanet, presumably Qatar-1b, is revealed in the analyzing results of the collected data, showing the validity of the transit approach for exoplanet detection. By using this approach, exoplanets planets can be discovered for further research in regards to potentially habitable and/or resource-rich exoplanets.
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