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中央研究院天文及天文物理研究所
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行星科學

Probability map of the fraction of symmetric island twotinos (fS) and asymmetric twotinos in the leading island (fL), constrained by the observed population fractions of the symmetric and leading asymmetric islands ( fS,OSSOS, fL,OSSOS; i.e., the number of detections in each island should be the same as the ratio in the OSSOS sample). The rejected regions for this probability distribution are indicated with solid (99% confidence level) and dashed (95% confidence) white curves. Note that the absolute probabilities (color map) are low only because the cells have very high resolution; the contours correctly enclose the normalized probabilities. The fS and fL from Chiang & Jordan (2002), Li et al. (2014), Pike & Lawler (2017), and Lawler et al. (2019) are overplotted with dots and labeled.
Constraining Migration Models with the 2:1 Resonance
Rotation period and spin rate vs diameter for the FOSSIL JTs (orange dots). The same is shown for previously measured JTs (green dots) and MBAs as well (the background gray dots). The green, orange, and blue dashed lines indicate rotation periods of 5, 4, and 3 hr, respectively. Note that only the objects with full and half derived rotation periods in our samples are used in this plot. All half periods are doubled for comparison to objects with full periods.
The spin-rate limit of Jupiter Trojans
Rotation period and spin rate vs diameter for the FOSSIL JTs (orange dots). The same is shown for previously measured JTs (green dots) and MBAs as well (the background gray dots). The green, orange, and blue dashed lines indicate rotation periods of 5, 4, and 3 hr, respectively. Note that only the objects with full and half derived rotation periods in our samples are used in this plot. All half periods are doubled for comparison to objects with full periods.
The spin-rate limit of Jupiter Trojans
Lightcurves of an occultation of a background star by Pluto observed on 15 Aug. 2018 at OAN, SPM in Baja California, México. The lightcurves were collected at a cadence of 20 Hz using two of the TAOS II telescopes, one with a commercial Andor Zyla CMOS camera (grey) and one with the TAOS II prototype CIS107 CMOS camera (blue). The spikes in the middle of occultation event, which are consistent in both light curves, are scintillation events stemming from density waves in the atmosphere of Pluto.
Pluto Occultation 2018
Spectral energy distribution (wavelength vs. flux density) of the debris disc host star HD 105. Data points are coloured by wavelength regime: green for optical/near-infrared, blue for mid-infrared (including the Spitzer/IRS spectrum), and red for far-infrared (Herschel/PACS). White data points are ancilliary data, including ALMA 1.3mm and ATCA 9mm observations. Grey lines denote a grid of dust models (grain size and distribution) fitted to the data to determine the best-fit dust properties for the system.
Spectral energy distribution
ALMA Band 6 (1.3mm) naturally weighted image of HD 105, a young pre-main sequence star with a bright debris disc. The disc is spatially resolved, with a radius of ~ 80 au.
A Young Solar System Analogue Imaged by ALMA
Plot of distance vs. disc radius for a sample of 97 spatially resolved debris discs. The colour of each data point denotes the photospheric temperature of the host star. The size of each data point denotes the fractional width (dR/R) of the disc, assuming it is a Gaussian annulus. The black line denotes the limit at which a disc could be resolved by the Herschel satellite observatory. The small black dots denote discs with fractional widths of 0.1, 0.3, 0.5, and 1.0, respectively.
Disc radius as a function of stellar distance
Plot of stellar luminosity vs. disc temperature for a sample of 97 spatially resolved debris discs, taken from Marshall et al. (2021a). The dust temperature is plotted as a ratio with the blackbody temperature (i.e. Tdust/Tbb) at the observed location of the dust disc around each star. A general trend can be seen that the disc temperature tends toward the blackbody temperature for more luminous stars. This indicates that the dust grains responsible for the observed emission are larger around more luminous stars, as expected from dust grain removal through radiation pressure.
Dust temperature vs. stellar luminosity
Plot of stellar luminosity vs. disc radius for a sample of 97 spatially resolved debris discs, taken from Marshall et al. (2021a). The vertical error bars denote the width of the debris disc. Light grey lines denote samples randomly drawn from the posterior probability distribution of a power law fit to the distribution. An increasing trend between disc radius and stellar luminosity is observed, suggesting that larger discs are (generally) found around more luminous stars. The slope of this trend is what would be expected if the CO ice line in primordial protoplanetary discs were responsible for setting the location for planetesimal formation around the host stars.
A Trend in Stellar Luminosity-Disc Radius
The number of new visible Jupiter Family Comets (JFCs) produced by each mean motion resonance (MMR) with Neptune, in our numerical simulations including the 34 largest dwarf planets (DPs, red line) or only the giant planets (black line).
Contribution of several MMRs populations to the production of JFCs
A figure representing the different possible combinations of the contributions of each of the three populations of the Kuiper belt (Classical, Resonant, and Scattering), to the total Jupiter Family Comet (JFC) production.
Number of cometary nuclei required to sustain a population of JFCs in steady state.
Diffusion is computed after a frequency analysis of thousands of test particles. Bluer colors are for stable orbits, redder colors indicate unstable ones.
Diffusion map around the small moon Aegaeon (Saturn LIII).
g-r and r-z photometry of TNOs, showing the 3 unique surface types revealed by these three bands.
TNO surface colors in g, r, and z bands
The three TAOS II enclosures at San Pedro Mártir Observatory.
TAOS II enclosures at San Pedro Mártir Observatory
TAOS II telescope at Site #2.
TAOS II Telescope.
Weather map of the transiting hot Jupiter HD 189733b, illustrated by air pressure (color) and wind velocity fields (arrows), as viewed by someone who descends through the planetary atmosphere. The patters are generated primarily by equatorial Rossby waves on the highly irradiated planet. These waves lead to the equatorial super-rotating circulation, which reduces the day-night temperature contrast of this tidally locked exoplanet. The circulation model also explains why the maximum thermal flux from the planet occurs several hours before secondary eclipse, an observational result revealed by the Spitzer Space Telescope (Tsai, Dobbs-Dixon, Gu, ApJ, 2014, 794, 141).
Weather on a Hot Jupiter
Orbit diagram of the planetary system surrounding the K-dwarf star HD 40307. The grey area indicates the star's habitable zone. Notice that the outermost planet is right in the habitable zone.
A super Earth in the habitable zone_animation gif
A back-scattered image of the E44 CAI from the CV3 Efremovka chondrite taken on a scanning electron microscope. This CAI is of particular interest because of the first demonstration of the former existence of short-lived 41Ca (t1/2 = 0.1 Myr). Reanalysis of potassium isotopes of this CAI (on the dark-gray minerals, named fassaite) resulted in a lower initial ratio of 41Ca/40Ca in the solar system from 1.4e-8 to 2.6e-9. A factor of 5 difference has an important implication for the origin of 41Ca and of the solar system.
A back-scattered image of the E44 CAI from the CV3 Efremovka chondrite taken on a scanning electron microscope
This isochron diagram shows the inferred 41Ca/40Ca ratio in the E44 CAI from the Efremovka meteorite. 20 years ago, the former existence of 41Ca (half-life = 0.1 Myr) was first demonstrated in this CAI, with the inferred 41Ca/40Ca ratio = 1.4e-8 (long dashed line). Reanalysis of K isotopes in the same CAI with an advanced secondary ion mass spectrometer revealed a 5-time lower 41Ca/40Ca ratio of 2.6e-9. This discovery has important implications for the origin of short-lived radionuclides in the early solar System.
A new initial abundance of 41Ca in the early solar system
Inferred 26Al/27Al ratios for spinel-hibonite spherules from Murchison and Paris and the probability density plot derived from the data. The overall 26Al/27Al range in the two groups of SHIBs is essentially identical, from ~1E−5 up to 6E−5. Three distinctive peaks can be identified in the probability plot at 26Al/27Al=4.9E−5, ~3.5E−5 and 6.5E−5, respectively. Two barely resolved components at 6E−5 and 2.5E−5 are also revealed.
The distribution of 26Al/27Al in spinel-hibonite spherules extracted from CM chondrites

中研院天文及天文物理研究所(ASIAA)的行星科學團隊參與許多太陽系及其他恆星相關 的廣泛研究課題，包含了理論模型與觀測，並且持續的成長。

對於太陽系相關的研究，ASIAA 在兩項大型巡天計劃中扮演著主導角色。 The Transneptunian Automated Occultation Survey(TAOS II) II)主要致力於測量海王星外天體 (TNO) 和內奧爾特雲(Inner Oort Cloud)中天體的大小分佈。 TAOS II 將在墨西哥下加利福 尼亞州的 聖佩德羅馬蒂爾天文台 運轉。該巡天將使用三台1.3公尺的 望遠鏡，以 20 Hz 的觀測頻率，同時觀測多達 10,000 顆恆星，以解析由直徑 300 公尺 < D < 30 公里 的 TNO 造成的短期掩星事件（200 毫秒）。即使使用現今最大的望遠鏡，這些天體也因為 太暗而無法直接觀察到。然而，測量這些物體的大小分佈對於我們理解太陽系的形成 和演化至關重要。此外，這些觀測目標也是木族彗星 (Jupiter Family Comets, JFC) 最可 能的來源，這些天體的普查對於了解 TNO 遷移到彗星軌道的動力學過程至關重要。

除 TAOS II 外，ASIAA 也是FOSSIL Survey (Formation of the Outer Solar System: An Icy Legacy)計劃的主要合作夥伴。 FOSSIL這個特別的計劃為台灣、日本、韓 國、中國、新西蘭、加拿大和美國的國際合作計劃，將利用夏威夷的昂望遠鏡 (Subaru telescope) telescope)的廣角相機 Hyper Suprime-Cam (HSC) 來做觀測。該計劃將覆蓋 105 平方度， 結合巡天特徵參數，偵測暗至r = 27等的太陽系小天體，例如 TNO、木星特洛伊小行星 (Jupiter Trojans, JTs)、希爾達小行星(Hildas)、主帶和近地小行星(MainBelt and Near Earth Asteroids)。該計劃的第一階段，將試圖測量 JTs 和 Hildas 的自旋速率，以及測量 TNO、JT 和 Hildas在暗端的大小分佈。此觀測覆蓋 30平方度。以高觀測頻率去觀測木星 拉格朗日點 L4 和 L5 的位置，找尋並統計 JTs 和 Hildas 的自旋速率以了解它們的內部結 構（單一結構或是小石堆的聚合體），以及檢測較暗的 TNO。計劃的第二階段，將聚焦 在為期三年，涵蓋75平方度，並且探測暗至26等TNO的巡天調查。藉由這些物體三年以 上的觀測，以得到它們較精準的軌道參數，進而分析它們的動力學分類。此計劃也將進 行天體的表面顏色測量，結合大小分佈和動力學分類，研究團隊將能提供支持或反對 第九行星假設的證據，也可利用不同 TNO 動力學分類提供對於太陽系形成歷史的證據 ，並且約束海王星遷移模型及TNO 的碰撞歷史。

行星科學團隊的成員也正在進行外太陽系的大規模動力學模擬。 特別是對於海王星外 的矮行星 (Dwarf Planets, DP) 的動力學影響研究。與僅考慮與海王星引力相互作用相比 ，它們增加了 TNO 進入彗星軌道的遷移率。 此外，這些矮行星也造成許多 TNO 軌道 的長期不穩定，導致它們被拋出太陽系。另外，對半人馬小行星(Centaurs)的類似模擬 也顯示，其中一些天體與木星和土星處於穩定的三體共振狀態，除此之外，土星衛星 的模擬軌道，特別是 Pallene，也正在確認它們的共振結構。

在我們的太陽系之外，ASIAA 行星科學團隊也正在進行主題相當廣泛的研究，包含原 行星和岩屑盤到具有系外行星和系外衛星的演化系統。 利用阿塔卡馬大型毫米/亞毫米 陣列 (Atacama Large Millimeter/submillimeter Array, ALMA) 對原行星盤的觀測，能夠 發現和並校正這些結構中的各種特徵，例如氣環、螺旋流入、壓力顛簸和盤偏心。 其 中一些特徵可能與行星形成過程密切相關，因此盡可能的了解這些特徵至關重要。

行星科學團隊的成員也參與了許多碎片盤研究方面的研究。使用地面和太空觀測，如 ALMA、赫歇爾太空望遠鏡(Herschel space observatory 、哈伯太空望遠鏡(Hubble Space Telescope, HST)、甚大望遠鏡(Very Large Telescope, VLT)的光譜偏振高對比度儀器 (SPHERE)，對單個原行星系統的結構進行詳細的多波長研究。利用已經空間解析出的盤 面系統特徵，拼湊它們的演化過程，並尋找原恆星/盤面特性的相關趨勢。在結合輻射 傳遞模型和實驗室塵埃測量，對組成塵埃顆粒（和原行星物質）的組成進行建模，追踪 原行星影響下的動力學演化，並且在疏散星團附近的年輕恆星周圍尋找系外彗星及其 原行星帶。

最後，在演化的行星系統領域也有許多重要的研究正在進行。建立FGKM 矮恆星周圍行 星形成和演化的模型，以解釋 Kepler/K2 數據，並對加法夏望遠鏡 (CFHT) 上的極化紅外 光譜議 (SPIRou) 做相關科學準備。利用熱潮汐理論檢驗是否可以解釋異常大的熱木星 。對短週期系外行星形成的模擬，進行共軌行星的預測，並且延伸此研究，檢查在來 自Kepler/K2 或凌日系外行星巡天衛星 (Transiting Exoplanet Survey Satellite, TESS) 的數據 ，確認發現此類行星系統的可能性。其他研究著重於系外衛星，特別是發展用於判斷 Kepler/K2 和 TESS 數據中系外衛星信號的新方法，以及使用 HST 或詹姆斯·韋伯太空望 遠鏡 (James Webb Space Telescope, JWST) 進行有目標性的觀測。近期的工作還包括多 衛星行星凌日時間變化的建模和推論。

研究人員 (17)

尚賢 Shang, Hsien cv 研究員
研究興趣: 理論及計算天文物理，恆星及行星形成，磁流體動力學，噴流，隕石
王祥宇 Wang, Shiang-Yu cv 研究員
研究興趣: 可見光與紅外線儀器，半導體元件
林明楷 Lin, Min-Kai cv 副研究員長聘
研究興趣: 天文物理流體力學，主要應用於行星形成及演化論
辜品高 Gu, Pin-Gao cv 副研究員
研究興趣: 系外行星，原始行星盤，星際衝擊波
溫志懿 Wen, Chih-Yi cv 研究技師
研究興趣: 儀器控制, 程式設計, 高能物理
汪仁鴻 Wang, Jen-Hung cv EPO主管, 研究助技師
研究興趣: 可見光天文學，太陽系小型天體，掩星技術，天體軌道計算，太陽系星曆
管一政 Kuan, Yi-Jehng cv 研究員; 師大地科系合聘
研究興趣: 天文化學，分子天文物理，分子雲及天文生物學
章展誥 Chang, Rex Chan-Kao cv 訪問學者
馬恩迪 Marshall, Jonathan cv 國科會研究學者
研究興趣: 岩屑盤和系外行星
陳英同 Chen, Ying-Tung cv 支援科學家
研究興趣: 可見光資料處理/太陽系天文物理
戈葆拉 Granados Contreras, Agueda Paula cv 支援科學家
研究興趣: 系外行星、行星動力學、行星形成與演化
黃鍾凱 Huang, Chung-Kai cv 支援科學家
研究興趣: 太陽系, 海王星外天體, 掩星, 天文資料模型, 時域天文學, 光變曲線
金升光 King, Sun-Kun cv 計畫支援
研究興趣: 量子光學與量子測量、 衛星系統工程（軌道分析）、 古柏帶天體與掩星觀測
歐碁爾 Otten, Gilles Peter Paul Louis cv 支援科學家
研究興趣: 光學和紅外線儀器, 系外行星
張智威 Zhang, Zhi-Wei Kiwi cv TAOS 支援工程師/科學家
研究興趣: 天文影像處理、程式語言撰寫
齊孝嵐 Teachey, Alexander cv 博士後研究學者
研究興趣: 系外行星和系外衛星
連馬修 Lehner, Matthew cv TAOS計畫首席科學家
研究興趣: 可見光天文學

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