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Page 1: Black holes: Introduction. 2 NS to BH 1209.0783 The authors studied collapse from NS to BH. Calculations were done for two cases: with and without massive

Black holes: Introduction

Page 2: Black holes: Introduction. 2 NS to BH 1209.0783 The authors studied collapse from NS to BH. Calculations were done for two cases: with and without massive

2

NS to BH

1209.0783

The authors studied collapse from NS to BH.Calculations were done for two cases:with and without massive (7%) disc.If a disc is present then such objectscan appear as sGRB.GW signal is weak, and so they area subject for the third generation of detectors.

Page 3: Black holes: Introduction. 2 NS to BH 1209.0783 The authors studied collapse from NS to BH. Calculations were done for two cases: with and without massive

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Main general surveys

• astro-ph/0610657 Neven Bilic BH phenomenology

• astro-ph/0604304 Thomas W. Baumgarte BHs: from speculations to observations • hep-ph/0511217 Scott A. Hughes Trust but verify: the case for astrophysical BHs

• arXiv: 0907.3602 Josep M. Paredes Black holes in the Galaxy

• arXiv: 1003.0291 S.-N. Zhang Astrophysical Black Holes in the Physical Universe

• arXiv: 1501.02937 Alister W. Graham  Galaxy bulges and their massive black holes

• arXiv: 1312.6698 Ramesh Narayan, Jeffrey E. McClintock  Observational Evidence for Black Holes

Page 4: Black holes: Introduction. 2 NS to BH 1209.0783 The authors studied collapse from NS to BH. Calculations were done for two cases: with and without massive

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BHs as astronomical sources

• Primordial BHs. Not discovered, yet. Only upper limits (mostly from gamma-ray observations). • Stellar mass BHs. There are more than twenty good candidates in close binary systems. Accretion, jets. Observed at all wavelenghts. Isolated stellar mass BHs are not discovered up to now. But there are interesting candidates among microlensing events. • Intermediate mass BHs. Their existence is uncertain, but there are good candidates among ULX. Observed in radio, x-rays, and optics.• Supermassive BHs. There are many (dozens) good candidates with mass estimates. In the center of our Galaxy with extremely high certainty there is supermassive BH. Accretion, jets, tidal discruptions of normal stars. Observed at all wavelenghts.

Page 5: Black holes: Introduction. 2 NS to BH 1209.0783 The authors studied collapse from NS to BH. Calculations were done for two cases: with and without massive

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Page 6: Black holes: Introduction. 2 NS to BH 1209.0783 The authors studied collapse from NS to BH. Calculations were done for two cases: with and without massive

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Что такое черная дыра?

Для физика Для астронома

Компактное (размер горизонта)массивное тело, не проявляющее признаков наличия поверхности,и чьи недра недоступны для наблюдений.

Объект, обладающий горизонтом.

Обладает определенными внутренними свойствами

Обладает определеннымивнешними проявлениями

Page 7: Black holes: Introduction. 2 NS to BH 1209.0783 The authors studied collapse from NS to BH. Calculations were done for two cases: with and without massive

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Коллапс облака

Мы всегда видим часы в центре, но они все краснее и краснее…

Page 8: Black holes: Introduction. 2 NS to BH 1209.0783 The authors studied collapse from NS to BH. Calculations were done for two cases: with and without massive

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Горизонты

Теорема об отсутствии волос: «Черные дыры не имеют волос».Черная дыра полностью описываетсямассой и вращением.

Page 9: Black holes: Introduction. 2 NS to BH 1209.0783 The authors studied collapse from NS to BH. Calculations were done for two cases: with and without massive

9L. Baiotti, Rezzolla et al.

Page 10: Black holes: Introduction. 2 NS to BH 1209.0783 The authors studied collapse from NS to BH. Calculations were done for two cases: with and without massive

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Коллапс

L. Baiotti, Rezzolla et al.

Page 11: Black holes: Introduction. 2 NS to BH 1209.0783 The authors studied collapse from NS to BH. Calculations were done for two cases: with and without massive

11Giacomazzo, Rezzolla et al.

Page 12: Black holes: Introduction. 2 NS to BH 1209.0783 The authors studied collapse from NS to BH. Calculations were done for two cases: with and without massive

12Giacomazzo, Rezzolla et al.

Page 13: Black holes: Introduction. 2 NS to BH 1209.0783 The authors studied collapse from NS to BH. Calculations were done for two cases: with and without massive

13Giacomazzo, Rezzolla et al.

Page 14: Black holes: Introduction. 2 NS to BH 1209.0783 The authors studied collapse from NS to BH. Calculations were done for two cases: with and without massive

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The most certain BH – Sgr A*

(see the reference in gr-qc/0506078)

Stellar orbits from 1992 till 2007

arXiv: 0810.4674

Page 15: Black holes: Introduction. 2 NS to BH 1209.0783 The authors studied collapse from NS to BH. Calculations were done for two cases: with and without massive

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... and it becomes more and more certain

See the reference in gr-qc/0506078New data in arXiv: 0810.4674Recent review - 1311.1841

Observations are going on.So, the number of stars with well measured orbits grows.

MBH ~ 4-5 106 Msolar

Page 16: Black holes: Introduction. 2 NS to BH 1209.0783 The authors studied collapse from NS to BH. Calculations were done for two cases: with and without massive

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Stellar mass BHs.The case of solar metallicity.

(Woosley et al. 2002)

BHs are formed by massive stars.The limiting mass separating BH and NS progenitors is not well known.In addition, there can be a range ofmasses above this limit in which, again,NSs are formed (also, there can bea range in which both types ofcompact objects form).

See 1011.0203 about progenitors

Page 17: Black holes: Introduction. 2 NS to BH 1209.0783 The authors studied collapse from NS to BH. Calculations were done for two cases: with and without massive

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Supernova progenitors

1011.0203

However, there are claimsthat most of stars >18M0

produce BHs(see a review in SmarttarXiv: 1504.02635)

Page 18: Black holes: Introduction. 2 NS to BH 1209.0783 The authors studied collapse from NS to BH. Calculations were done for two cases: with and without massive

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Which stars form BHs?

1409.0006

It is proposed that stars with compact internal structure (M~20-30 Msolar) form BHs not NSs. This expains data on RGs and the SN rate.

Page 19: Black holes: Introduction. 2 NS to BH 1209.0783 The authors studied collapse from NS to BH. Calculations were done for two cases: with and without massive

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Mass spectrum of compact objects

(Timmes et al. 1996, astro-ph/9510136)

Results of numerical models

Page 20: Black holes: Introduction. 2 NS to BH 1209.0783 The authors studied collapse from NS to BH. Calculations were done for two cases: with and without massive

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BH mass function

1006.2834

Likelihood based on 16 systems

Page 21: Black holes: Introduction. 2 NS to BH 1209.0783 The authors studied collapse from NS to BH. Calculations were done for two cases: with and without massive

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BH mass distribution

1011.1459

Page 22: Black holes: Introduction. 2 NS to BH 1209.0783 The authors studied collapse from NS to BH. Calculations were done for two cases: with and without massive

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A NS from a massive progenitor

(astro-ph/0611589)

Anomalous X-ray pulsar in the cluster Westerlund1most probably has a very massive progenitor, >40 MO.

Page 23: Black holes: Introduction. 2 NS to BH 1209.0783 The authors studied collapse from NS to BH. Calculations were done for two cases: with and without massive

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Stellar mass BHs. The case of zero metallicity

(Woosley et al. 2002)

Pop III massive stars couldproduce very massive BHs whichbecame seeds for formationof supermassive BHs.

Page 24: Black holes: Introduction. 2 NS to BH 1209.0783 The authors studied collapse from NS to BH. Calculations were done for two cases: with and without massive

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BHs and NSs in close binary systemsStudying close binaries with compact objects we can obtain

mass estimates for progenitors of NSs and BHs (see, for example, Ergma, van den Heuvel 1998 A&A 331, L29).

An interesting result was obtained for the NS system GX 301-2. The progenitor mass was found to be equal to 50 solar masses or more.On the other hand, for many systems with BHs estimates of progenitor masses are lower: 20-50 solar masses.

Finally, for the BH system LMC X-3 the mass of the progenitor is estimated as >60 solar masses.

So, the situation is rather complicated.Most probably, in some range of masses, at least in binary systems,both variants are possible.

Page 25: Black holes: Introduction. 2 NS to BH 1209.0783 The authors studied collapse from NS to BH. Calculations were done for two cases: with and without massive

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Binary evolutionA BH can be formed even from stars each below the limit.

Page 26: Black holes: Introduction. 2 NS to BH 1209.0783 The authors studied collapse from NS to BH. Calculations were done for two cases: with and without massive

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“Scenario machine” calculations

Page 27: Black holes: Introduction. 2 NS to BH 1209.0783 The authors studied collapse from NS to BH. Calculations were done for two cases: with and without massive

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GRBs and BHs

According to the standard modern model of long GRBs, a BH is the main element of the “central engine”.

So, studying GRBs we can hope to get important informationabout the first moments of BH’s life.

See a very brief review inarXiv:1302.6461

Page 28: Black holes: Introduction. 2 NS to BH 1209.0783 The authors studied collapse from NS to BH. Calculations were done for two cases: with and without massive

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BHs from GW signalsLIGO and VIRGO will measure signalsfrom compact object mergers.

Some of them can be due to NS+BH,or BH+BH mergers.

These signals can be more powerfuldue to larger masses. So, even beingrarer per unit volume, they can be morefrequent in the data.

Page 29: Black holes: Introduction. 2 NS to BH 1209.0783 The authors studied collapse from NS to BH. Calculations were done for two cases: with and without massive

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NS and BH coalescenceNumerical models show (astro-ph/0505007, 0505094) that such eventsdo not produce GRBs

BH-NS mergers are still a popular subject of studies:1105.3175, 1103.3526, 1210.8153, 1302.6297, 1301.5616, 1304.3384.

Page 30: Black holes: Introduction. 2 NS to BH 1209.0783 The authors studied collapse from NS to BH. Calculations were done for two cases: with and without massive

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Magnetic field jet launch

1410.7392

Neutron star magnetic field helps to launch the jet. But disc is still necessary!

Page 31: Black holes: Introduction. 2 NS to BH 1209.0783 The authors studied collapse from NS to BH. Calculations were done for two cases: with and without massive

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Prompt mergers of NSs with BHs

(astro-ph/0505094)

Coleman Miller demonstrated that in NS-BH coalescence most probably there isno stable mass transfer andan accretion disc is not formed.This means – no GRB!

The top solid line is constructed by assuming that the neutron star will plunge when, in one full orbit, it can reduce its angular momentum below the ISCO value via emission of gravitational radiation.The next two solid lines reduce theallowed time to 30 and 10% of an orbitThe bottom line ignores gravitationalradiation losses entirely.

Page 32: Black holes: Introduction. 2 NS to BH 1209.0783 The authors studied collapse from NS to BH. Calculations were done for two cases: with and without massive

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Extremal BH-NS mergersIt is possible to form a disc around a BH during BH-NS merger, but only in caseof extreme parameters. For example, extreme BH rotation.

1302.6297

Page 33: Black holes: Introduction. 2 NS to BH 1209.0783 The authors studied collapse from NS to BH. Calculations were done for two cases: with and without massive

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SupernovaeThe neutrino signal during a (direct) BH formation must be significantly differentfrom the signal emitted during a NS formation. (arXiv: 0706.3762)

Constant growth of neutrino energy and a sharp cut-off indicate a BH formation.Result depends on the EoS.

Different curves are plotted for different types of neutrino:electron – solid, electron anti-neutrino – dashed, mu and tau-neutrinos – dot dashed.

See some new results in: arXiv:0809.5129   BH formation in a PNS collapse and neutrino spectra

Page 34: Black holes: Introduction. 2 NS to BH 1209.0783 The authors studied collapse from NS to BH. Calculations were done for two cases: with and without massive

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BH signatures in SN light curves

Balberg, Shapiro astro-ph/0104215

(see also Zampieri et al., 1998, ApJ 505, 876)

For this plot no radioactive heatingis taken into account.

An accreting BH can “emerge”after ~few months-years.

Page 35: Black holes: Introduction. 2 NS to BH 1209.0783 The authors studied collapse from NS to BH. Calculations were done for two cases: with and without massive

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New calculations

1401.3032

Several mechanisms of energy release are calculated:

• “accretion heating” (solid line)

• neutrino annihilation (dotted line)

• Blandford-Znajek emission (dashed line).

Estimates show that fallback can potentially lead to large amount of energy deposition to the ejecta, powering super-luminous supernovae.

Page 36: Black holes: Introduction. 2 NS to BH 1209.0783 The authors studied collapse from NS to BH. Calculations were done for two cases: with and without massive

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A BH birth???

0912.1571

Page 37: Black holes: Introduction. 2 NS to BH 1209.0783 The authors studied collapse from NS to BH. Calculations were done for two cases: with and without massive

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Conclusions• There can be different kinds of BHs: PBH, stellar, IMBH, SMBH• Stellar mass BHs can be observed due to - accretion in binaries - GRBs - GW - in SN• Mass interval for stellar mass BH formation is not certain


Seed BH formation via direct collapse Kazu Omukai （ Tohoku ） Major contributers Kazu Sugimura (Tohoku) Kohei Inayoshi （ Columbia ） Takashi Hosokawa （ Tokyo

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