ライフサイエンスコーパス: black hole

1 ~10(4) Schwarzchild radii for a 10(9)M((.)) black hole).

2 he Sun (and that the supernova left behind a black hole).

3 ly two neutron stars or a neutron star and a black hole).

4 s a few hundred gravitational radii from the black hole.

5 a spinning [Formula: see text]62 solar mass black hole.

6 events during S0-2's closest approach to the black hole.

7 see text] solar masses, which can only be a black hole.

8 ates that the gas is relatively close to the black hole.

9 ase powered by accretion onto a supermassive black hole.

10 rks within protons or the event horizon of a black hole.

11 etry for the fast-moving clouds close to the black hole.

12 bserved in a rare and transient stellar-mass black hole.

13 was recently found near the Galactic Centre black hole.

14 % of the gravitational radius of its central black hole.

15 mising seed for the formation of a monstrous black hole.

16 gas towards the galactic centre to feed the black hole.

17 to radio flux ratios required for accreting black holes.

18 not show evidence for accreting supermassive black holes.

19 ction between stellar-mass and super-massive black holes.

20 terpret this as the dynamical imprint of the black holes.

21 black holes and hyper-accreting stellar-mass black holes.

22 mpact objects currently interpreted as being black holes.

23 ential and forms accretion disks around both black holes.

24 ingredient in regulating mass accretion onto black holes.

25 f detecting gravitational waves from merging black holes.

26 critical accretion onto massive stellar-mass black holes.

27 d lead to some hosting multiple supermassive black holes.

28 properties not seen in Galactic stellar-mass black holes.

29 fall (the Eddington limit) onto stellar-mass black holes.

30 mical objects such as accretion disks around black holes.

31 anglement monogamy, such as those arising in black holes.

32 ation about the physical properties of their black holes.

33 ated quantum systems and information loss in black holes.

34 he tidal disruption of a star by the central black hole(1,2).

35 n of gas into disks surrounding supermassive black holes(1-3).

36 a powerful tool for characterizing chaos in black holes(1-4).

37 l Eddington limit, or onto intermediate-mass black holes (10(3)-10(5) solar masses).

38 has been thought to be an intermediate-mass black hole (100 to 10,000 solar masses) because of its e

39 that the disk extends nearly to the central black hole(14,15).

40 few hundreds of gravitational radii from the black hole(17,18).

41 ional waves(1) and in the first imaging of a black hole(2).

42 accretion disk formed around the newly born black hole(7-10) as the dominant source of heavy r-proce

43 life with a catastrophic collapse to leave a black hole-a promising seed for the formation of a monst

44 How black holes accrete surrounding matter is a fundamental

45 Energy output from a black hole accreting at a low rate has been proposed, bu

46 black holes or as emission from stellar-mass black holes accreting above their Eddington limit, analo

47 Microquasars are stellar-mass black holes accreting matter from a companion star and e

48 io'), which is an important parameter of the black hole accretion process.

49 ations show that these cold clouds also fuel black hole accretion, revealing 'shadows' cast by the mo

50 ing the period of maximal star formation and black hole activity.

51 Intense star formation and supermassive black-hole activity is occurring within the galaxies emb

52 phase of rapid accretion onto a supermassive black hole, an unknown mechanism must remove or heat the

53 information processing and investigation of black hole analogs in controllable quantum systems.

54 ruption event involving an intermediate-mass black hole and a white dwarf(13).

55 ale magnetic field that is advected from the black hole and distorted by dissipation processes within

56 bjects, all lying within 0.04 parsecs of the black hole and forming a class that is probably unique t

57 o provide the feedback required by models of black hole and host galaxy coevolution.

58 s on physical models of accretion physics in black hole and neutron star binary systems.

59 growth of black holes and the coevolution of black holes and galaxies.

60 nd explaining the close relationship between black holes and galaxies.

61 redicted by models of accreting supermassive black holes and hyper-accreting stellar-mass black holes

62 smology and underlies our description of the black holes and neutron stars that are ultimately respon

63 between quantum models on graphs and quantum black holes and suggest methods to experimentally study

64 s to theories of the formation and growth of black holes and the coevolution of black holes and galax

65 to affect the evolution of both supermassive black holes and their host galaxies, quenching star form

66 hole (within the sphere of influence of the black hole), and that it can be swept away even at low r

67 elled from the accretion disk encircling the black hole, and collimated radio jets.

68 within the innermost hundred parsecs of the black hole, and falling closer towards it.

69 ecause most large galaxies contain a central black hole, and galaxies often merge, black-hole binarie

70 y the accretion disk than by the spin of the black hole, and if the baryons can be accelerated to rel

71 inosity is released as matter falls onto the black hole, and radiation-driven winds can transfer most

72 arly stage of the jet, closer to its central black hole, and show that the prompt phase is produced v

73 ive of growth by coherent accretion for this black hole, and suggests that black-hole growth at 0.5 <

74 ions, are inconsistent with EOR galaxies and black holes, and are largely explained by IHL emission.

75 the nature of gravity and the properties of black holes, and in 2017 electromagnetic observations of

76 itational sphere of influence of the central black holes, and interpret this as the dynamical imprint

77 ical states plays a key role in the study of black holes, and our work simulates such nontrivial stru

78 flows inwards towards accretion disks around black holes, and such an inflow has been measured at the

79 Accreting black holes are known to power relativistic jets, both i

80 spin orientations (that is, the spins of the black holes are randomly oriented with respect to the or

81 At z > 2, supermassive black holes are thought to grow mostly by merger-driven

82 e, with low natal kicks (the velocity of the black hole at birth) and restricted common-envelope evol

83 nt to which the activity of the supermassive black hole at the center of the Milky Way, known as Sagi

84 When a supermassive black hole at the centre of a galaxy accretes matter, it

85 t superposition models to determine that the black hole at the centre of NGC 1600 has a mass of 17 bi

86 Activity from the super-massive black hole at the Galactic Centre, which is coincident w

87 relativistic outflows (jets) from accreting black holes at cosmological distances.

88 Eddington limit, analogous to some Galactic black holes at peak luminosity.

89 Accreting supermassive black holes at the centres of active galaxies often prod

90 es that of the Sun to the billion-solar-mass black holes at the centres of galaxies.

91 Quasars are rapidly accreting supermassive black holes at the centres of massive galaxies.

92 e been attributed to primordial galaxies and black holes at the epoch of reionization (EOR) or, alter

93 ULXs are usually modeled as stellar-mass black holes (BHs) accreting at very high rates or interm

94 Mass accretion by black holes (BHs) is typically capped at the Eddington r

95 Accreting black holes (BHs) produce intense radiation and powerful

96 are expected to be radiated by supermassive black hole binaries formed during galaxy mergers.

97 Galaxy mergers produce supermassive black hole binaries, which emit gravitational waves prio

98 entral black hole, and galaxies often merge, black-hole binaries are expected to be common in galacti

99 m a minority of the total population of star-black-hole binaries(5,6).

100 an about 10 seconds) often observed in other black-hole binaries-for example, XTE J1118+480 and GX 33

101 Black hole binary systems with companion stars are typic

102 If the orbital period of the black-hole binary matches this value, then for the range

103 om accretion of cooling gas onto the central black hole, but requires an accretion rate finely tuned

104 of mass determination for intermediate-mass black holes, but has hitherto not been realized.

105 dust; by the gravitational potential of the black hole; by radiative feedback; or by the interplay b

106 In contrast to many other systems, a black hole can never be isolated from its Hawking radiat

107 sible solution to the paradox if evaporating black holes can actually be described in terms of standa

108 ical active galactic nuclei with higher-mass black holes can be expected to exhibit high-amplitude op

109 ry of the accretion flow around stellar-mass black holes can change on timescales of days to months(1

110 is key to understanding whether supermassive black holes can grow from stellar-mass black holes or wh

111 The tidal forces close to massive black holes can rip apart stars that come too close to t

112 Tidal forces close to massive black holes can violently disrupt stars that make a clos

113 ted X-ray emission lines from a more typical black-hole candidate X-ray binary, 4U 1630-47, coinciden

114 f mass [Formula: see text] M ( ), implying a black hole companion of [Formula: see text] M ( ).

115 s comparable to freefall speeds close to the black hole, constraining the fastest infalling gas to wi

116 wever, whether below z approximately 1 these black holes continue to grow by coherent accretion or in

117 alos, even those hosting active supermassive black holes, contrary to some previous results.

118 One more binary black-hole detection and a significant candidate event d

119 arameters for each of the four likely binary black hole detections GW150914, LVT151012, GW151226 and

120 Near a black hole, differential rotation of a magnetized accret

121 When a black hole emerges from quiescence (that is, it 'turns o

122 ommon and if the field continues to near the black hole event horizon, disk structures will be affect

123 ional interpretation as energy flux across a black hole event horizon.

124 via thermal instability and accrete onto the black hole exhibit the necessary tuning.

125 oretical studies have difficulty growing the black hole fast enough.

126 ly the keys that will allow us to understand black hole feedback on the largest scales over cosmologi

127 acteristics of the jets and distributing the black-hole feedback more uniformly over the surrounding

128 Most binary black holes form without supernova explosions, and their

129 window into the environments in which binary black holes form.

130 We report numerical simulations of early black hole formation starting from realistic cosmologica

131 emitted from gas that is accreting onto the black hole from a companion star.

132 clumpy accretion flow towards a supermassive black hole fuel reservoir in the nucleus of the Abell 25

133 predict the properties of subsequent binary-black-hole gravitational-wave events.

134 re of the gaseous fuel reservoirs that power black hole growth is nevertheless largely unconstrained

135 etion for this black hole, and suggests that black-hole growth at 0.5 </= z </= 1 occurs principally

136 f its current age-reinforces models of early black-hole growth that allow black holes with initial ma

137 basis of a near-infrared spectrum) that the black hole has a mass of approximately 1.2 x 10(10) M Su

138 erger of two massive (about 30 solar masses) black holes has been detected in gravitational waves.

139 f the flow, which for accreting stellar-mass black holes has shown evidence for precession(1) due to

140 ' descendants of this population of 'active' black holes have been found in the galaxies NGC 3842 and

141 Black holes have been predicted to radiate particles and

142 All stellar-mass black holes have hitherto been identified by X-rays emit

143 Observations of stellar-mass black holes, however, reveal equivalent (mass-scaled) re

144 parsecs of the Milky Way host a supermassive black hole identified with the position of the radio and

145 ion to emission line reverberation masses of black holes if they are calibrated against the two objec

146 three or fewer gravitational radii from the black hole, implying a spin parameter (a measure of how

147 s have been placed on the mass of a putative black hole in 47 Tucanae (NGC 104) from radio and X-ray

148 Here we show there is evidence for a central black hole in 47 Tucanae with a mass of solar masses whe

149 Accretion onto the supermassive black hole in some active galactic nuclei (AGN) drives r

150 The existence of an intermediate-mass black hole in the centre of one of the densest clusters

151 this conjecture by calculating the mass of a black hole in the corresponding quantum mechanical syste

152 iction and confirm the existence of a binary black hole in the relativistic regime.

153 a non-local superposition of a Schwarzschild black hole in two distinct locations-due to its Hawking

154 With the first direct detection of merging black holes in 2015, the era of gravitational wave (GW)

155 peak of their accretion phase, supermassive black holes in galactic cores are known to emit very hig

156 n of black holes that grow into supermassive black holes in galaxies.

157 Supermassive black holes in galaxy centres can grow by the accretion

158 e thought to fuel the growth of galaxies and black holes in massive protoclusters.

159 tion of previously unrecognized supermassive black holes in other ultra-compact dwarf galaxies.

160 determine the masses of central supermassive black holes in such galaxies.

161 promising being heating by the supermassive black holes in the central galaxies, through inflation o

162 ck loop is the process by which supermassive black holes in the centres of galaxies may moderate the

163 The origin of super-massive black holes in the early universe remains poorly underst

164 the main driver of the formation of massive black holes in the early Universe.

165 Supermassive black holes in the nuclei of active galaxies expel large

166 The majority of the accreting supermassive black holes in the Universe are obscured by large column

167 s is connected to the growth of supermassive black holes in their centers.

168 n, there would be major voids, the infamous "black holes", in our immune repertoire.

169 For the use of the black-hole indicator dye, the calix[4]pyrrole was modifi

170 from within a few gravitational radii of the black hole ionizing the disk wind hundreds of gravitatio

171 m the galaxy's low-level active supermassive black hole is capable of driving the observed wind, whic

172 Although the black hole is essentially quiescent in the broader conte

173 lectromagnetic counterpart suggests that the black hole is not accreting at a sufficient rate to make

174 When the black hole is not accreting gas, it can be found through

175 from close to the event horizon and that the black hole is rapidly spinning.

176 a spin parameter (a measure of how fast the black hole is rotating) of a = 0.87(+0.08)(-0.15) at the

177 However, the existence of intermediate-mass black holes is still uncertain, and their formation proc

178 A remarkable yet mysterious property of black holes is that their entropy is proportional to the

179 es between obscured and unobscured accreting black holes is therefore their mass-normalized accretion

180 established method of measuring the spin of black holes is through the study of relativistic reflect

181 disk in the hard-X-ray state of stellar-mass black holes is truncated at a few hundreds of gravitatio

182 Accretion of matter onto black holes is universally associated with strong radiat

183 tidal disruption of a star by a supermassive black hole leads to a short-lived thermal flare.

184 nt black holes, non-enhanced lesions and non-black hole lesions, a task yet to be demonstrated by oth

185 assuming standard scaling of timescales with black hole mass and accretion properties, typical active

186 The high black hole mass and mass fraction suggest that M60-UCD1

187 Assuming the black hole mass indicated by host galaxy scaling relatio

188 of only two active galactic nuclei for which black hole mass measurements based on emission line reve

189 or stellar-mass black holes, we estimate the black hole mass of M82 X-1 to be 428 +/- 105 solar masse

190 ing of the B9Ia donor star, we constrain the black hole mass to be less than 15 solar masses.

191 stable and scale in frequency inversely with black hole mass with a reasonably small dispersion.

192 oximately 1.4-fold increase in the dynamical black hole mass, implying a corresponding correction to

193 10(13) times the luminosity of the Sun and a black-hole mass of 8 x 10(8) solar masses.

194 These systems are all binaries with a black-hole mass that is less than 30 times that of the S

195 than 10(40) ergs per second), which require black hole masses of 50-100 times the solar value or sig

196 this value, then for the range of estimated black-hole masses, the components would be separated by

197 We find that the seeds of massive black holes may be much more common than previously cons

198 th the statistically less significant binary black hole merger candidate LVT151012.

199 ically proving the connection between binary black hole mergers and active galactic nuclei as hosts,

200 gravitational waves from stellar-mass binary black hole mergers by the Laser Interferometer Gravitati

201 bed by binary black hole observations.Binary black hole mergers have recently been observed through t

202 Probing the origin of binary black hole mergers will be difficult due to the expected

203 detected gravitational waves from two binary black hole mergers, GW150914 and GW151226, along with th

204 were discovered with the detection of binary black-hole mergers and they should also be detectable fr

205 lculations predict detections of about 1,000 black-hole mergers per year with total masses of 20-80 s

206 clusters are a primary formation channel for black-hole mergers(11-13), but the rates and properties(

207 produces approximately 40 times more binary-black-holes mergers than do dynamical formation channels

208 This intermediate-mass black hole might be a member of an electromagnetically i

209 ng discovery of a coalescing pair of "heavy" black holes (more massive than [Formula: see text] M[For

210 ying gadolinium-enhanced lesions, persistent black holes, non-enhanced lesions and non-black hole les

211 of astrophysical questions probed by binary black hole observations.Binary black hole mergers have r

212 There is a supermassive black hole of mass 4 x 10(6) solar masses at the centre

213 ygni, an X-ray transient source containing a black hole of nine solar masses (and a companion star) a

214 ctivity-effort space produces the hyperbolic black hole of NPs, where IMPs populate the high-effort b

215 ccretion close to the Eddington limit onto a black hole of stellar mass.

216 alogues of quasars that contain supermassive black holes of 10(6) to 10(10) solar masses.

217 Gravitational-wave experiments have detected black holes of similar mass, but the formation of such m

218 Newly formed black holes of stellar mass launch collimated outflows (

219 y regions of the early Universe; yet dormant black holes of this high mass have not yet been found ou

220 h redshifts greater than z = 6 suggests that black holes of up to ten billion solar masses already ex

221 hase in the accretion flow around a low-mass black hole (of approximately 4 x 10(5) solar masses) wit

222 th strong magnetic fields, onto stellar-mass black holes (of up to 20 solar masses) at or in excess o

223 Our ability to simulate black holes offers the potential to further explore the

224 n of gravitational waves from merging binary black holes opens up a window into the environments in w

225 ched from white dwarfs, and an origin from a black hole or a neutron star is hard to reconcile with t

226 icating that it is a noninteracting low-mass black hole or an unexpectedly massive neutron star.

227 ions of binary stars containing an accreting black hole or neutron star often show x-ray emission ext

228 eted either as evidence of intermediate-mass black holes or as emission from stellar-mass black holes

229 rise because of the presence of supermassive black holes or result from a non-standard stellar initia

230 ssive black holes can grow from stellar-mass black holes or whether a more exotic process accelerated

231 energy dissipation occurs ~1 parsec from the black hole (or ~10(4) Schwarzchild radii for a 10(9)M((.

232 spheres of compact objects (neutron stars or black holes) or relativistic shocks launched from such o

233 There has been much debate over whether black-hole orbits could be smaller than one parsec.

234 triple black hole systems, with the closest black hole pair being 2.4 kiloparsecs apart (the third c

235 hancing and/or new T2 lesions into permanent black holes (PBH); magnetisation transfer ratio (MTR) of

236 y interacting with the supermassive Galactic black hole, possibly enhancing its accretion activity.

237 owever, have not sampled the relevant binary-black-hole progenitors--massive, low-metallicity binary

238 are one of the main ways in which accreting black holes provide kinetic feedback to their surroundin

239 e other is modified with a spectrally paired black-hole quencher (BHQ).

240 of an inherently fluorescent guest dye or a black-hole quencher from the receptor's cavity by means

241 relativistic velocities are associated with black holes ranging in mass from a few times that of the

242 on limit, theoretical models have focused on black hole rather than neutron star systems.

243 Direct-collapse black holes-remnants of supermassive stars, with masses

244 ission from the Galactic Center supermassive black hole, Sagittarius A*.

245 p potential well of the central supermassive black hole, Sagittarius A*.

246 Here we consider the decoherence of a "black hole Schrodinger cat"-a non-local superposition of

247 that a star passing close to a supermassive black hole should exhibit a relativistic redshift.

248 Intermediate-mass black holes should help us to understand the evolutionar

249 Supermassive black holes (SMBHs) and their host galaxies are generall

250 Most supermassive black holes (SMBHs) are accreting at very low levels and

251 o frame-dragging effects that occur when the black-hole spin axis is misaligned with the orbital plan

252 ere we report that, if the magnitudes of the black hole spins are allowed to extend to high values, t

253 ironments is the angular distribution of the black hole spins.

254 riapse, where the tidal interaction with the black hole stretches them along the orbit) and they show

255 Here we report observations of a triple black hole system at redshift z = 0.39, with the closest

256 -ray, and radio observations of the Galactic black hole system V404 Cygni, showing a rapid synchrotro

257 Previous searches for compact black hole systems concluded that they were rare, with t

258 There are four known triple black hole systems, with the closest black hole pair bei

259 of X-ray reverberation lags in supermassive black-hole systems(12,13) suggest that the corona is com

260 electromagnetically invisible population of black holes that grow into supermassive black holes in g

261 The origin of the supermassive black holes that inhabit the centres of massive galaxies

262 lti-wavelength survey of hard-X-ray-selected black holes that reveals that radiative feedback on dust

263 ount of hot gas in the accretion zone of the black hole-that is, within 10(5) Schwarzschild radii (0.

264 to within 10,000 gravitational radii of the black hole (the gravitational radius being the gravitati

265 resulting stellar debris spirals toward the black hole, the debris heats up and emits x-rays.

266 ed by the accretion of material onto massive black holes; the detection of highly luminous quasars wi

267 Here we report X-ray observations of the black-hole transient MAXI J1820+070(19,20).

268 In particular, black-hole transients have outflows whose properties are

269 been reported in the transient stellar-mass black hole V404 Cygni, and interpreted as disrupted mass

270 erally believed that matter is absorbed into black holes via accretion disks, the state of which depe

271 rical simulations of the formation of binary black holes via the evolution of isolated binary stars,

272 The classical field formation of binary black holes we propose, with low natal kicks (the veloci

273 rse-mass scaling that holds for stellar-mass black holes, we estimate the black hole mass of M82 X-1

274 For stellar-mass black holes, we know that the high-frequency quasi-perio

275 The existence of this supermassive black hole when the Universe was only 690 million years

276 The existence of such black holes when the Universe was less than one billion

277 s per second towards the active supermassive black hole, which serves as a bright backlight.

278 supermassive (more than 10(9) solar masses) black holes, which probably affect the properties of the

279 with accretion-state changes of stellar mass black holes, which suggests that all TDFs could be accom

280 should be expected in any strongly accreting black hole whose spin is misaligned with the inflowing g

281 data reveals the presence of a supermassive black hole with a mass of 2.1 x 10(7) solar masses.

282 Each quasar contains a black hole with a mass of about one billion solar masses

283 The Galactic Centre contains a supermassive black hole with a mass of four million Suns(1) within an

284 chanism for feeding the central supermassive black hole with gas.

285 The co-evolution of a supermassive black hole with its host galaxy through cosmic time is e

286 sphere of influence (about 100 parsecs for a black hole with mass one billion times that of the Sun).

287 a long-speculated, supercritically accreting black hole with optically thick outflows.

288 trongly influenced by the interaction of the black hole with the enhanced gas density present within

289 involve a binary system of two supermassive black holes with a subparsec separation.

290 models of early black-hole growth that allow black holes with initial masses of more than about 10(4)

291 It has long been suspected that black holes with masses 100 to 10,000 times that of the

292 t to be powered by the accretion of gas onto black holes with masses of approximately 5-20M cicled do

293 Supermassive black holes with masses of millions to billions of solar

294 stellar systems containing a neutron star or black hole, with gamma-ray emission produced by an inter

295 launched from the innermost regions near the black hole, with the most powerful emission occurring wh

296 e, unbiased and complete sample of accreting black holes, with reliable information on gas column den

297 ens of parsecs of the accreting supermassive black hole (within the sphere of influence of the black

298 dates recent predictions that massive binary black holes would constitute the first detection.

299 ppear to be normal accreting neutron-star or black-hole X-ray binaries, but they are located in old s

300 n-on a time scale of minutes to hours-in the black-hole X-ray binary V404 Cygni, detected with very-l