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TMT Exoplanet Detection and Characterization周济林 (Ji-Lin Zhou)

Nanjing University, zhoujl@nju.edu.cn

transit spectroscopy for XO-2. credit ESA

Credit: TMT science

What TMT can do in exoplanet

1、Protoplanetary Disk

2、Detection & transit follow-up of Exoplanet

RV, image (Dou’s report)

3、Characterization --atmosphere

Focus on Chinese Exoplanet detection projects

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TMT Science book

1.Protoplanetary disk

Science: Planet formation: Gravitational instability or core accretion?

Disk evolution Gap opening & planet migration

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MIRES (Mid-Infrared Echelle Spectrometer): is a diffraction-limited, high-resolution (5000 < R < 100000) spectrometer and imager operating at 8 – 18 μm. a separate AO system optimized forthe mid-infrared.NIRES (Near-Infrared Echelle Spectrometer): fed by NFIRAOS, NIRES is a diffraction-limited high resolution(20 000 < R < 100 000) spectrometer covering 1 – 2.4 μm simultaneously.

Map out the velocity of disk

(1) gravitational instability model

Boss A.

Classical Planet Formation Scenario

HR 8799 system

<1Form MMSN:

(2) Core accretion model

Formation of km size

planetesimals

Accretion of planetesimals

into planetary embryos

Gas accretion, giant impact

www.planet.sci.kobe-u.ac.jp

type-II migration

planet’s perturbation

viscous diffusion

type-I migration

disk torque imbalance

Disk-planet tidal interactions

viscous disk accretion

Goldreich & Tremaine (1979), Ward (1986, 1997), Tanaka et al. (2002)

Lin & Papaloizou (1985),....

See, Kley et al. 2012 Annu. Rev. Astron. Astrophys.

2.Exoplanet detection (RV)

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HROS (High-Resolution Optical Spectrometer): a single-object, seeing-limited, high-resolution (R = 50000 for 1 arcsec slit) optical-UV echelle spectrographAdvantage : short time to get high SNRScience :(1)Down to M,L type stars (HZ more close)(2)RM-effect(3)Transit Follow (Kepler, TESS,…)Tusk: target list (from transit)

HD: 67 Me /113 MeJup: <12Me/320Me

J

Udry & Santos 2007

Tidal inflation?

Charbonneau et al. Nature 2009

III-2. Internal structure and atmosphere of planets

Batalha et al. 2012, 1202.585216 Months of Kepler Data

total: 2300 planets, 20% of the stars catalogued have multiple planets. paucity of giant planets at short periods in multiple planet systems.

Need choose targets!

3. Exoplanet atmosphere

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Task:(1)More simulation:--planet radius, location

(2)Make a list for suitable candidates(3)Habitable Earth?

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2.16m(NAOC) 2.4m (YNO)

AST3

Chinese Planet Search Projects

BSST(?)

SDUO

南大 ,国台 ,紫台等合作

2008 data: Total of ~20,000stars, we choose ~10000 stars with precision of <2%, We find 10 most-promising candidates.

CSTAR-1P=2.04 days

R~0.5RJThe binned phase-folded light curve (top panel) along with the normalized BLS periodogram (bottom panel) of one CSTAR object. The solid line in the top panel

show the best-fit transit model

Photometric accuracy

Frequency of Exoplanets

1% 0.047%

0.5% 0.085% N:0.038%

0.1% 0.28% sE:0.233%

According to Kepler’s results (transiting, P<100 days)

Submitted to ApJS

CSTAR数据 : 发现了 56颗双星 -星表

我们使用 CSTAR2008年观测数据进行细致的光变分析，从 10,000个源中找到56颗双星并整理成双星星表，包括 15个不相接双星、 6 个半接双星、 27个密近双星和 8 个未分类的可疑双星。我们还对不相接双星计算了掩星中心时刻的变化。我们将我们的结果与 Kepler发现的双星系统做了轨道参数的统计性比较，二者有相同的分布趋势。我们发现 5 颗双星处于近相接演化阶段， 3 颗双星具有较大偏心率，并且发现一颗双星同时具有大偏心率与明显的掩星中心时刻变化。这些结果对双星系统的形成和演化提供了重要的参考价值。

Yang Ming, Zhang Hui & Zhou Ji-Lin*, Zhou Xu, Liu Hui-Gen, Wang Lifang, et al., Eclipsing Binary Stars from 14.5cm Telescope at Dome A Antactica, in preparing;

南大 ,国台 ,紫台

Conclusion

To join in TMT in exoplanet:

(1) Group too small and weak, more persons need to be trained:

Disk, RV, transit, exoplanet

(2) Preliminary tusk should be assigned soon

(3) Sent young persons abroad to learn

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