ライフサイエンスコーパス: black hole

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

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

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

4 ase powered by accretion onto a supermassive black hole.

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

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

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

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

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

10 was recently found near the Galactic Centre black hole.

11 % of the gravitational radius of its central black hole.

12 n disk in a prograde orbit around a spinning black hole.

13 axy offer a powerful probe of a supermassive black hole.

14 to 4000 kilometers per second to the merged black hole.

15 oximately 3,100 Schwarzschild radii from the black hole.

16 bris that forms an accretion disk around the black hole.

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

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

19 ingredient in regulating mass accretion onto black holes.

20 f detecting gravitational waves from merging black holes.

21 critical accretion onto massive stellar-mass black holes.

22 d lead to some hosting multiple supermassive black holes.

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

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

25 shone brightly as a result of accretion onto black holes.

26 ng in bright flares from otherwise quiescent black holes.

27 in a total population of approximately 5-100 black holes.

28 M22 could arise from heating produced by the black holes.

29 by the accretion of matter onto supermassive black holes.

30 r masses are the elusive 'intermediate-mass' black holes.

31 to radio flux ratios required for accreting black holes.

32 not show evidence for accreting supermassive black holes.

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

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

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

36 mpact objects currently interpreted as being black holes.

37 ential and forms accretion disks around both black holes.

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

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

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

41 gorous star formation is not observed around black holes above an X-ray luminosity of 10(44) ergs per

42 How black holes accrete surrounding matter is a fundamental

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

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

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

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

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

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

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

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

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

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

53 f X-ray-emitting binary stars comprising one black hole and one other star ('black-hole/X-ray binarie

54 he tight correlation between the mass of the black hole and the mass of the stellar bulge results fro

55 e black-hole merging process, through binary black holes and final collapse into a single black hole

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

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

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

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

60 approximately ten solar mass 'stellar mass' black holes and the 'supermassive' black holes of millio

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

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

63 ties, and broad implications of stellar-mass black holes and ultraluminous x-ray sources.

64 anding the life cycles of these supermassive black holes (and vice versa).

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

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

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

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

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

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

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

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

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

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

75 The masses of supermassive black holes are known to correlate with the properties o

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

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

78 These two black holes are significantly more massive than predicte

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

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

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

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

83 Pairs of quasars, each with a massive black hole at the centre of its galaxy, have separations

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

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

86 Ongoing searches for intermediate-mass black holes at galaxy centres will help shed light on th

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

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

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

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

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

92 tute the bulges of galaxies, and the massive black holes at their centres, are the relics of a period

93 that all massive galaxies have supermassive black holes at their centres.

94 We find that most copiously accreting black holes at these epochs are buried in significant am

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

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

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

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

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

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

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

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

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

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

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

110 Therefore, black holes coevolve only with bulges.

111 s driven by global processes, so the biggest black holes coevolve with bulges, but growth of the latt

112 When black holes collide, their tendexes and vortexes interac

113 high ratio of radio-to-X-ray flux for these black holes, consistent with the larger predicted masses

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

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

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

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

118 We conclude that black holes do not correlate directly with dark matter.

119 ion of this galaxy, and the closeness of the black holes embedded in the bulge, provide a hitherto mi

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

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

122 g observational point to the study of galaxy/black hole evolution.

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

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

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

126 uggest that there are two different modes of black-hole feeding.

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

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

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

130 k holes reflects the behavior of the massive black holes found by astronomers and described by classi

131 who have tried to understand the behavior of black holes from a quantum mechanical point of view, how

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

133 Black holes generate collimated, relativistic jets, whic

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

135 Our results imply that black holes grow in tandem with their host galaxies thro

136 ere we report a measurement of the amount of black hole growth in galaxies at redshift z = 6-8 (0.95-

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

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

139 t in Henize 2-10 indicates that supermassive black-hole growth may precede the build-up of galaxy sph

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

141 The black hole has a mass of about two million solar masses,

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

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

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

145 Black holes have been predicted to radiate particles and

146 Although a few black holes have been seen in globular clusters around o

147 Supermassive black holes have powerful gravitational fields with stro

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

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

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

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

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

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

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

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

156 that have been established for stellar-mass black holes in binary systems in the past decade and a h

157 In contrast, small black holes in bulgeless galaxies and in galaxies with p

158 A description based on string theory and black holes in five dimensions has made the quark-gluon

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

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

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

162 nsistent with the larger predicted masses of black holes in globular clusters compared to those outsi

163 How jet physics scales from stellar black holes in GRBs to the supermassive ones in AGN is s

164 The identification of two black holes in one cluster shows that ejection of black

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

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

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

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

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

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

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

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

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

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

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

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

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

178 holes in one cluster shows that ejection of black holes is not as efficient as predicted by most mod

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

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

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

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

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

184 As the young star approaches the black hole, its disc experiences both photoevaporation a

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

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

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

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 olating the widely used correlations between black-hole mass and the stellar velocity dispersion or b

194 10(13) times the luminosity of the Sun and a black-hole mass of 8 x 10(8) solar masses.

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

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

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

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

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

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

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

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

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

206 The final stages of the black-hole merging process, through binary black holes a

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

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

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

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

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

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

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

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

215 lar mass' black holes and the 'supermassive' black holes of millions to billions of solar masses are

216 ter M22, and we argue that these objects are black holes of stellar mass (each approximately 10-20 ti

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

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

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

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

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

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

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

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

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

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

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

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

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

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

231 Hundreds of stellar-mass black holes probably form in a typical globular star clu

232 ong-term accretion onto central supermassive black holes, produce relativistic jets with lifetimes of

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

234 report the use of a nonfluorescent quencher (Black Hole Quencher, BHQ) as an acceptor for smFRET.

235 odified at its 5' and 3' ends with QDs and a black hole quencher, respectively.

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

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

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

239 The popular conception of black holes reflects the behavior of the massive black h

240 he system and/or the spins of the individual black holes results in an enhanced Poynting flux.

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

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

243 s; this is because the initial conditions of black hole seed properties are quickly erased during the

244 discovered plunging towards the supermassive black hole, SgrA*, at the centre of the Milky Way.

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

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

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

248 Supermassive black holes (SMBHs; mass is greater than or approximatel

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

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

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

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

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

254 cy of energy dissipation in jets produced in black hole systems is similar over 10 orders of magnitud

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

256 from curved spacetime, that are attached to black holes: tendexes, which stretch or squeeze anything

257 etermined, and some may be intermediate-mass black holes that form through exotic mechanisms.

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

259 tar can be used as a marker for supermassive black holes that otherwise lie dormant and undetected in

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

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

262 ng the channels of formation of the earliest black holes; this is because the initial conditions of b

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

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

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

266 ximately 10(4)-10(5) M(middle dot in circle) black holes via the direct collapse of gas.

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

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

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

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

271 uggests that the progenitors of supermassive black holes were formed as approximately 10(4)-10(5) M(m

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

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

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

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

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

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

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

279 2-10 harbours an actively accreting central black hole with a mass of approximately one million sola

280 laxies typically contain a centrally located black hole with a mass that is millions or even billions

281 2, a star orbiting our Galaxy's supermassive black hole with a period of just 11.5 years.

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

283 black holes and final collapse into a single black hole with gravitational wave emission, are consist

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

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

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

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

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

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

290 Although some black holes with masses more than 10(9) times that of th

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

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 mprising one black hole and one other star ('black-hole/X-ray binaries') in Milky Way globular cluste