Title ブラックホールと重力波天文学 Author(s) 長峯, 健太郎 Citation 高大連携物理教育セミナー報告書. 28 Issue Date Text Version publisher URL DO

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1 Title ブラックホールと重力波天文学 Author(s) 長峯, 健太郎 Citation 高大連携物理教育セミナー報告書. 28 Issue Date Text Version publisher URL DOI rights Osaka University Knowledge Archive : OUKA Osaka University

3 (BH), LIGO

4 Black Hole (BH) Laplace : 17, John Mitchell Pierre Laplace John Wheeler black hole BH (black)!! Wheeler

5 Escape Velocity r 2GM v esc = r

6 Event Horizon BH Event horizon : =

7 Schwarzchild Radius r 2GM R s = c 2 3 km BH Rs = 3 km x (M/M ) M Msun= Karl Schwarzchild

8 (TOV limit) Gravity singularity

9 BH Andrew Hamilton s page: tidal force( (Time dilation)

10 Black Hole Mass( ). (Kepler s 3rd law) BH TOV limit (~3 M ) BH.

11 X-ray Binary X X 3 M BH 10 M. X-ray binary: Cygnus X-1 TOV limit 18 MSun BH 10 MSun

12 (General Relativity): R µ 1 2 Rg µ + g µ = 8 G c 4 T µ credit: NASA Albert Einstein (1879~1955) (space-time)

13 LIGO (Laser Interferometer Gravitational Wave Observatory)

15 circular orbits assumed for the waveform phase & amplitude important ~10 cycles followed

16 GW (Sep 14, 2015)

17 Initial BH masses: Final BH mass: (source frame) Distance: Radiated energy in GW: Source localization: 590 deg 2 final spin: Dim-less spin param:

PSR B1913+16 Orbital decay of binary pulsar (neutron star) (Hulse & Taylor 75) (Taylor &

20 PSR B Orbital decay of binary pulsar (neutron star) (Hulse & Taylor 75) (Taylor & Weisberg 82) source: Nobel Foundation 93 First indirect evidence of GW emission Weisberg & Taylor 04

21 Astrophysical Implication ( 25M ) BHs. (~10 Gyr).. (metallicity 0.5Z ) BH : Gpc -3 yr -1 (comoving)

22 Bouwens+ 09 Kistler+ 13

24 How does a high-mass star die?

25 Core runs out of fuel!.. Gravity ( ) wants to collapse the star!

26 Death of High-Mass Stars The core and outer layers run out of fuel... The star then collapses, due to gravity. The mass is high enough that nothing (even the degeneracy pressure) can balance the gravitational collapse.

27 Death of High-Mass Stars Gravity ( ) wants to collapse the star No outward pressure = implosion Rebound of outer layers against the core = supernova

28 Supernova 1987A The closest supernova in the last four centuries was seen in 1987.

29 Supernovae Remnants Energy released by core collapse drives the outer layers into space the Crab nebula Remnant of the supernova seen in A.D neutron star in the center Xray view

30 What happens to the core after a supernova? Neutron Star heavy stars: remaining mass of 1.4 M to about 3 M Black Hole really heavy stars: remaining mass greater than 3 M TOV limit

31 Some supernova explosions produces black holes as a remnant. (movie)

32 Supermassive Black Hole (SMBH)

33 Milky Way 4 x 10 6 M SMBH

36 More evidence for supermassive black holes gas motion of ~100s km/s at <60 ly from the center M87 3x10 9 M SMBH

37 More evidence water maser (microwave amplification by stimulated emission by radiation) NGC 4258 BH mass: 3.9 x 10 6 M

38 Black Holes in Galaxies supermassive black holes. dormant ( ) SMBH. quasar-like.

39 Supermassive BH 10 9 M 10 6 M 10 3 M 10 6 M 10 9 M M Magorrian relation; Ferrarese+ 01;

43 BICEP2 collaboration B

45 E E

46 BICEP

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Title 名詞型助数詞の用法 : 準助数詞セットと組を中心に Author(s) 東条, 佳奈 Citation 阪大日本語研究. 27 P.109-P.136 Issue 2015-03 Date Text Version publisher URL http://hdl.handle.net/11094/51518 DOI Rights Osaka