InterStellar_GW

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1 인터스텔라 영화속의 시공간과 중력파 부산대학교 물리학과 이창환 1

2 2017 Nobel Prize in Physics

3 KIP THORNE Caltech - (1997) LIGO (1992) (2009~)

4 KIP THORNE EXECUTIVE DIRECTOR OF INTERESTELLAR 2005 / 2006, (14 ) 2010 / /

5 영화는 영화다 - THIS IS NOT POSSIBLE. - NO, IT IS NECESSARY. 비유는 비유다 - 내용은 정확한가 - 제대로 전달되고 있는가 주요 참고문헌 The Science of Interstellar (Kip Thorne, 2014) Black Holes & Time Warps (Kip Thorne, 1994) 블랙홀전쟁 (서스킨드/이종필, 2011) Figures from Interstellar, Wikipedia, NASA/ESA, 5

6 4 GARGANTUA / A 5 / / 6

7 7 4

8 8

9 9

10 - - ` ` 10

11 10 23 cm 10 9 cm 10 2 cm Image by kip Thorne cm cm 11

12 Image by kip Thorne 12

13 / 1915 ( ) 13

14 NASA/ESA / 14

15 / ( -133 ) 3, 15

16 GPS ( ) 16

17 17 GARGANTUA

18 GARGANTUA The Life of Gargantua and Pantagruel Pentalogy written by Francois Rabelais, 16th century Pantagruel ( ) : son of Gargantua 18

19 블랙홀 발견 XTEJ Centaurus A 은하중심 거대 블랙홀 블랙홀 쌍성 / 강한 엑스선방출 2002 노벨물리학상 19 M87

20 GARGANTUA 1 / 1-7 : The Science of Interstellar 20

21 GARGANTUA 21

22 22

23 + = / cm (10-43 ) ( : cm) 3 / : 23

24 Preskill, Thorne, Hawking /, /, ! 24

25 10-33 cm (10-43 ) ( : cm) : < cm : < : 25

26 : cm : < cm : <

27 27 A

28 28

29 / M R 2 / 1 M M GARGANTUA R 29

30 The Science of Interstellar / singularity ( ) (GARGANTUA) BKL singularity ( ) Infalling singularity Outflying singularity TARS 30

31 BKL singularity Tesseract Tesseract / 4 The Science of Interstellar 31

32 TESSERACT - Tesseract / 4 = 8 3 The Science of Interstellar 32

33 중력을 통한 쿠퍼와 머피의 만남 머피의 방 력 중 3차원 공간 빛 / 3차원 진공 요동 The Science of Interstellar 33

34 34 5

35 2? 3? 2 3 ( ) 35

36 2 3. ( ) 4 5. ( ) 36

37 TARS 5 1AU ( 8 ) 1.5cm Gargantua GARGANTUA? 37

38 ~0 km 4 km? 38

39 39

40 - / (Ludwig Flamm) (Gannon & Lee) Kip Thorne Black Holes and Time Warps 40

41 Casimir : 41

42 10-33 cm (10-43 ) ( : cm) 42

43 43

45 - / (KGWG) 45

46 2019.!!! / 40 The Science of Interstellar 46

47 .. We will find a way. we always have. 47

48 ESA: Virgo Virgo-aVirgo-ET US: LIGO iligo-eligo-aligo Japan TAMA300-CLIO-KAGRA LIGO-India NSF (LIGO CLone) LIGO- India (Approved) Image credit: ( ) 48

49 Nd:YAG 1064nm ( ) 40kg (SiO2) ( 1ppm ) 49

50 GW propagating in z-direction line element ds 2 = dt 2 +(1+h + )dx 2 +(1 h + )dy 2 + dz 2 +2h dxdy Z p lengths in x- & y-directions (plus polarization) L x = Z x2 x 1 p 1+h+ dx ( h +)L x0 ; Z y p L y = Z y2 y 1 p 1 h+ dy (1 1 2 h +)L y0 plus polarisation h+ hx cross polarisation 50

51 What is interacting with GW, laser light or test mass? TT gauge - mirrors & beam splitters remain at rest - GW (h) interact with interferometer s light local Lorentz (LL) frame - in the proper reference frame of beam splitter - beam splitter is freely falling with GW - mirrors are moving - tiny correction due to GW & light interaction Kip Thorne physical observables should be independent of coord choice 51

52 4km (1 1/10 ) (20 W 700 W 100 kw) 280 4km ( : 200 W 750 kw) : 10 / 30 52

53 LIGO GW Detectors LIGO sensitivity h with 4km arms L L L m m How to measure m using laser with l 10 6 m? L l

54 Sensitivity of Interferometers If the length resolution is λlaser, detectable strain is h l l = laser l = 10 6 m 10 3 m = 10 9 Fabry-Perot cavity (~ 250 bounces) : GW 1000 km for 300 Hz h l l eff laser GW 10 6 m 10 6 m = Due to quantum nature of the photons, the length resolution could be reduced h 1 p Nphotons laser GW 54

55 Measuring the phase shift by averaging over some period τ Poisson distribution N = p N N: measured number of photons over period τ E = ~ 2 c N E = ~ 2 c p N l l Uncertainty in the phase measurement : =2 c t l t E ~ 2 1 p N t E = p l 2 c ~2 c ~ N l 2 N 1 2( ) 2 55

56 Shot noise Collect photons for a time of the order of the period of GW wave 1/f GW N photons = P laser hc/ laser P laser 1 hc/ laser f GW For 1W laser with λlaser=1 µm, fgw=300hz, Nphotons=10 16 h l l eff N 1/2 photons GW laser m 10 6 m = By adopting high power laser (20W for O1) and power recycling, we can reach astrophysical sensitivity of ~

57 Gw

58 Credit: NSF/LIGO/SSU/A.Simonnet Oct 16, 2017 GW from Binary NS Mergers GW GRB A by Fermi-GBM Kilonova/X-ray/Optical Afterglows

59 Multi-messenger Observation Binary Neutron Star Merger 59

60 :41:04 UTC 라이고및비르고중력파신호포착 +2 초후페르미및인티그랄감마선신호포착 KMTNet( 서울대 / 한국천문연구원 ) + 약 11 시간후칠레천문대망원경들이가시광선신호포착 + 약 21 시간후국내연구진호주이상각망원경으로추적관측시작. 이후약 4 주간추적관측 (KMTNet, BOOTES-5 망원경등 ) + 약 9 일후찬드라우주망원경 X- 선신호포착 + 약 16 일후지상전파망원경전파신호포착 그림출처 : LIGO, NASA, 1M2H/UC Santa Cruz and Carnegie Observatories/Ryan Foley, 서울대 / 한국천문연구원 / 임명신, NSF/Sonoma 주립대 /A. Simonnet, NRAO 서울대학교초기우주천체연구단 ( 임명신 )

61 61

62 ,,, / 62

63 Einstein Telescope (ESA) 2030? (designing stage) elisa km 10 km LISA pathfinder

64 LIGO Scientific Collaboration

현대대학물리학 12(415~456p)

현대대학물리학 12(415~456p) 시공간과 물질, 진동과 파동 상대성 원서 35장 그림 12.1 중심에 있는 은하의 중력렌즈 작용으로 형성된 머나먼 퀘이사의 영상을 보여 주는 아인슈타인의 십자가. 무엇을 배우는가 12.1 에테르 찾기 12.2 아인슈타인의 가설과 기준틀 베타와 감마 보기문제 12.1 아폴로 우주비행선 광원뿔 시공간 간격 12.3 시간팽창과 길이수축 시간팽창 보기문제 12.2