Wei Zhu(祝伟)
I'm now an Assistant Professor in the Department of Astronomy at Tsinghua University in Beijing.
祝伟
《观测宇宙学:从太阳系走向宇宙深处》讲座
2022年12月12日
本讲座在线PPT\(\uparrow\)
图片来源:ESA/Planck Collaboration
1亿光年
10万光年
1光天
(200天文单位)
系外行星研究可以解答的问题
原行星盘存在的时间
Image credit: C. Mordasini
(~1,000 km)
Terrestrial planets formed after the gaseous disk is gone, through collisions among protoplanets.
(磁)流体力学过程,星子形成
Gaseous planets formed within the disk lifetime
星子
原行星
(行星胚胎)
岩石行星
气态巨行星
失控气体吸积
大碰撞
白雪宁
* Ignoring the pulsar planets.
公转轨道半长轴(日地距离)
行星质量(地球质量)
公转轨道半长轴(日地距离)
行星质量(地球质量)
Image from NASA Exoplanet Archive
视向速度法
凌星法
微引力透镜法
直接成像法
Image from NASA Exoplanet Archive
年份
累计发现的系外行星数目
视向速度法
凌星法
微引力透镜法
直接成像法
人马座51行星
开普勒望远镜升空
Known planets around Sun-like stars, data from NASA Exoplanet Archive, figure adapted from Zhu & Dong (2021)
Transit (ground)
Transit (space)
Radial velocity
Microlensing
Imaging
'Pale Blue Dot' by Voyager 1 from 40 AU
半人马座\(\alpha\)星处 (1.3 pc)
旅行者1号“暗淡蓝点”照片
Earth: \(R_{\rm Earth}\), 300 K
100x\(R_{\rm Earth}\), 6000 K
10x\(R_{\rm Earth}\), 150 K
太阳亮度是地球的十亿倍!
(此外,行星离主星非常的近)
HR 8799: planet brightness ~\(10^{-5}\) star
b
c
d
e
\( \rightarrow\) 谱线移动约\(10^{-8}\)倍的波长
Image credit: ESO
\( \frac{v}{c} = \frac{\Delta \lambda}{\lambda} \)
王雪凇
自1990年代起,电荷耦合器件CCD和计算机的使用极大地提高了天文观测的精度和效率。
2019年诺贝尔物理学奖:"for the discovery of an exoplanet orbiting a solar-type star."
Didier Queloz
Michel Mayor
周期4.2天
热木星
冷木星
1%
10%
Image credit: LCOGT
探测要求:对大量恒星进行长时间、高精度的测光观测
公转周期 | 凌星深度 | 凌星时长 | |
---|---|---|---|
木星 | 13年 | 1% | 1天 |
地球 | 1年 | 0.01% | 12小时 |
轨道倾角\( i \lesssim R_\star/a = 1.7^\circ \left(\frac{a}{\rm AU}\right)^{-1} \)
K2 mission (2014-2019)
天鹅座和天琴座区域约100平方度
超级地球(super Earth)
K2 mission (2014-2019)
天鹅座和天琴座区域约100平方度
超级地球(super Earth)
郭守敬望远镜(LAMOST)
Berger et al. (2018)
LAMOST-Kepler Survey
California-Kepler Survey
Gaia mission
Mordasini et al. (2009) (see also Ida & Lin 2004)
超级地球
“冷”木星
热木星
公转轨道半长轴(日地距离)
行星质量(地球质量)
Super Earths
行星接收到的恒星的光/地球接收到的太阳的光
恒星温度
宜居带(乐观估计)
宜居带(保守估计)
每颗类太阳恒星拥有的宜居行星的数目
图片来源:Kunimoto & Matthews (2020)
不同的研究论文
系外行星研究可以解答的问题
Super Earths
Paczynski (1986); Mao & Paczynski (1991)
\(t_{\rm E} \sim 30{\rm days} \left(\frac{M_{\rm L}}{M_\odot}\right)^{1/2} \)
\( t_q \sim 40{\rm min} \left(\frac{q}{10^{-6}}\right)^{1/2} \left( \frac{t_{\rm E}}{30 \rm days}\right) \)
背景恒星亮度
背景恒星
”透镜“星体
\( t_{\rm E} \)
\( t_q \)
毛淑德
Figure from Zhu & Dong (2021)
Cold Neptunes
Animations from B. Scott Gaudi
银河系中心
1 deg
Credit to: KASI, Gould et al. (2020)
Figures from Suzuki et al. (2016)
(see also Gould et al. 2010, Cassan et al. 2012, Clanton & Gaudi 2014, Udalski et al. 2018, Jung et al. 2019)
Yee, Zang, et al. (2021)
5 hr
Figure from 臧伟呈
Transit (ground)
Transit (space)
Radial velocity
Microlensing
Imaging
Hot Jupiters
Cold Jupiters
Super Earths
Cold Neptunes
Figure from Zhu & Dong (2021)
公转轨道半长轴(日地距离)
行星质量(地球质量)
Hot Jupiters
1%
Cold Jupiters
10%
Super Earths
30%
Cold Neptunes
Figure from Zhu & Dong (2021)
Transit (ground)
Transit (space)
Radial velocity
Microlensing
Imaging
Figure adapted from Zhu & Dong (2021)
w/ known companions
w/o known companions
Hot Jupiters
Cold Jupiters
Super Earths
Cold Neptunes
Super Earths
Image credit: P. Armitage
Pebble (\(\sim\) cm)
Pebble isolation mass (\(\sim10\,M_\oplus\))
Chris Ormel
\( P({\rm SE}|{\rm CJ}) \cdot P({\rm CJ}) = P({\rm CJ}|{\rm SE}) \cdot P({\rm SE}) \) \( \rightarrow P({\rm SE}|{\rm CJ})=100\% \)
Cold Jupiters
Super Earths
22 from Kepler (triangles) + 39 from RV (squares)
(see also Batygin & Laughlin 2015)
\( P({\rm CJ,~no~SE}) = P({\rm CJ}) \cdot [1-P({\rm SE}|{\rm CJ})] \)
James Webb Space Telescope (exp. 2021.12.18)
詹姆斯·韦伯太空望远镜
Figures from Andrews (2020)
Atacama Large Millimeter/submillimeter Array (ALMA)
Figures from Andrews (2020)
Atacama Large Millimeter/submillimeter Array (ALMA)
中国太空站望远镜CSST、地球2.0凌星项目(ET)、近邻宜居行星巡天计划(CHES)、紫瞳、觅音、天邻
First detection: 1989/1995
# of detections: ~700
First detection: 2000
# of detections: >4000
# of detections: 0
(Gaia ~2024)
First detection: 2003
# of detections: ~50
Image from Dawson & Johnson (2018)
林潮(Doug Lin)
Fischer & Valenti (2005)
(see also Santos et al.2001, 2004, Ida & Lin 2004)
Formation of giant planet is sensitive to the amount of available solid material.
Holman & Murray (2005), Agol et al. (2005), Holman et al. (2010)
Figure from Hadden & Lithwick (2017)
(see also Wu & Lithwick 2011, Hadden & Lithwick 2014)
Transit singles have \(\sigma_e\approx0.3\), whereas transit multis have \(\sigma_e\approx0.05\) (Van Eylen et al. 2015, 2019, Xie et al. 2016, Mills et al. 2019).
Transit duration \(T\)
Zhu et al., 2018
(see also He et al. 2020)
\( \sigma_i,~\sigma_e \propto k^\zeta \)
Fulton et al. (2017)
Owen (2019)
(see also Owen & Wu 2017, Jin & Mordasini 2018)
Image credit: NASA
3'
9"
Images from Pietrukowicz et al. (2019)
Figure from Mao (2012)
Small-size stars
Intermediate-size stars
Large-size stars
Time in event unit
Magnification in brightness (log)
Transiting Exoplanet Survey Satellite
Huang et al., (2018) (see also Gandolfi et al. 2018)
Another similar system: HD 86226 (TOI-652.01)
Image credit: NASA/TESS
(Gaia+RV: Better characterization of Gaia multi-planet systems.)
By Wei Zhu(祝伟)
2021年秋季学期清华大学本科生通识课《观测宇宙学:从太阳系走向宇宙深处》讲座,约70分钟(含10-15分钟提问讨论)
I'm now an Assistant Professor in the Department of Astronomy at Tsinghua University in Beijing.