The black holes with the masses of the ordinary stars

Transcription

1 Th Black hls in th univrs, filld by th gasus dark mattr Srgy G. Burag D.Sc., Prf. Stat Univrsity f Arspac Tchnlgy, Mscw, Russia buragsg@yandx.ru Sit: Abstract This articl discusss sm f cntradictins in xplanatins th natur f black hls. It is shwn that th black hls with masss f rdinary stars ar unstabl. Thy shuld b dstryd by th actin f cntrifugal frcs. Th sizs f suprmassiv black hls in cntrs f spiral galaxis ar t larg. Bing f such sizs thy hav vry lw dnsitis. This cntradicts t th ida abut th black hls having th dnsitis f nutrn stars. Basd n th idas dvlpd in th thry f th gasus dark mattr [1,,] w hav rcivd mr ralistic sizs f th black hls. At such sizs thr ar n cntradictins in th mdrn thry f black hls.. In additin, in th articl is xplrd th rl f th black hls in th cycls f cnvrtin f a mattr and an nrgy in th univrs. It is shwn that th black hls in th cntrs f th spiral galaxis rprsnt hug "pt", which is th surcs f barynic mattr. Th dark mattr, which is absrbd frm surrunding spac, insid f th suprmassiv black hls is cnvrtd int barynic mattr, and thn is sprading in th vastnss f th univrs. In this cas, th black hls ar n lngr "singularitis." In th articl als it is shwn that tgthr with th dark mattr black hls gt trmndus nrgy. Calculatins shw that within 15 billin yars th suprmassiv black hls accumulat an nrgy, which is sufficint t xplain th bsrvd by astrnmrs th xplsins with rlas f nrmus nrgy, which cmmnsurat with an xplsin nrgy f all stars in galaxy. Th black hls with th masss f th rdinary stars Th stars calld f Black hls, which prsumably hav a big wight and a small siz (radii). Bcaus f this th wav f light (phtns n th chain lngth f th light wav.) can nt t vrcm a gravity and t lav a star. It is knwn that fr th car f n cmpnnt frm th binary systm f wights f its spd must t rach a crtain critical valu, calld th scap vlcity. This spd is dtrd by th frmula fm V (1) r W substitut th spd f light C m /c in this th xprssin instad f th spd f th star V. W slv it rlativly a stllar radius, w btain th valu f th gravitatinal radius f th star with a mass m : fm r C () If th radius f th star is lss than this valu, th light wav (a chain f a phtns n wavlngth f light) can nt t lav hr and th star shuld g ut frm th rst f th wrld. T s th "black hl" is impssibl. Thrfr, th attmpts t dtct thm rducd t finding a 1

2 scndary phnmna with an unusually strng gravitatinal intractins in th cntrs f th galaxis. Thugh th cnditin () is crrct, thr ar th dubts abut th pssibility f th xistnc f th black hls stars, satisfying this th cnditin. T s this, lt's apply it t a hypthtical star, frmd as a rsult f th cllaps f th nrmal stars with an initial paramtrs f th Sun (mass 0 6 1, m S kg radius r S m, th angular vlcity f rtatin ω,9 s ). Aftr th catastrphic cntractin f th star, ths paramtrs will chang at th paramtrs f 0 th black hl f th sam mass m kg, but with a smallr radius r m (frm quatin ). Frm th cnsrvatin f th angular mmntum w dfin a nw angular vlcity ωs rs 5 1 ω 1,6 s. Nxt, w calculat th avrag dnsity f th black hl r 0 m / 4 r 1, kg / m ρ π. It was in tims gratr than th dnsity f th atmic nuclus ( -particls), which is impssibl. W cntinu ur an analysis. Fr this w writ th cnditin f th dstructin f th black hl by th cntrifugal frcs. This will happn if th cntrifugal frc F xcds th frc f a gravity F F gr cnstant Fgr r f m T > 1 Th prid f th rtatin f th black hl f 11 6, N m / kg T π / ω S,915 5 () s. Th gravitatinal F. Fr ths valus th rati f ths quantitis is 5, 16. F As yu can t s, this a black hl in dystitln wuld b trn by th cntrifugal frcs. In th currnt ppular scintific litratur w can ftn t find th statmnt that th star with th sun paramtrs, can b cnvrtd int a black hl. This star rducs its th scp bfr f a thrkilmtr radius. But I hav nvr mt a cntinuatin f this th study, which wuld hav indicatd that such a star is unstabl and will b dstryd. In th prsnt thry f a dark mattr thr is th anthr rasn, which raisd a dubts n th xistnc f th stars black hls, satisfying th cnditin (). Th fact that th star is a black hl, lik any thr star, is a sink fr th dark gas. Th dark gas flws in th cntr f th star vnly alng th radius [1]. Thrfr, th phtns f a light hav t travl against th ncg flw. It rds whn a swimmr is swim n th rivr against th currnt. If th spd f th swimmr ds nt xcd th spd f th watr, h can t flat as lng as yu want, but h ds nt mv frward with rspct t th banks n n mtr. In viw f ths th cnsidratins, w bliv that th rat f th flw f th dark gas [1,], tward th star, nvr xcd th spd f a light C m / s which is mittd by th star. α m Vr < C (4) ρ r Accrding t [1,] th cfficint isα 1c 1. Whn this th cnditin is vilatd a star is bcms nt visibls. Th imum radius f th visibl stars is dtrd frm (4) α m f m r (5) ρ C α C Th imum radius f th star with th mass f th Sun, in which th star disappars frm viw accrding t xprssin (5), will b r 66,6 km. gr

3 Th valu f th imum radius r is th imum radius fr th stars with th mass f th Sun. It is th rdr valu f th radius that actually bsrvd stars such as th whit dwarfs. Th 0 smallst f th knwn whit dwarfs - th star Wlf 45 [9] has a lt f m 1,01 kg and th radius f r 40 km. r 00km. Th imum radius fr this mass accrding t th frmula (5) is Th Whit dwarf - th star Van Maann has th mass r 4900 km. Th imum radius fr this th star is r 50 km. Th Whit dwarf - th Sirius satllit has a mass m 0, 0 kg and th radius 0 m 1, kg and a radius r 0000 Th imum radius fr this th star is r 616 km. Thus it can b argud that th whit dwarfs ar nt far frm th thrshld f a visibility a stars. N wndr th astrnmrs can nt s th stars in th sky lss th rd and whit dwarfs. Th suprmassiv black hls in th cntrs f th spiral galaxis In th cntr f th spiral galaxy has bn fcus th cnsidrabl mass f th mattr, which crats a gravity twards th cntr f th galaxy. This frc kps a cg stars in thir rbits as thy rtat arund a cmmn cntr. Th stars mr distant frm th cntr hav incrasd th frc f a gravity f th mr nxt stars. Until rcntly, th astrnmrs blivd that in th cntrs f th galaxis ar th gas-dust cluds that d nt mit a light. It was assumd that in th cntr can b a star th light frm which is absrbd in th surrunding f th gas-dust cluds Tday th astrphysics sk t undrstand th stat f a mattr at th cntr f th galaxy. Th valu f th mass f a mattr in th cntr was dtrd frm th analysis f th dynamics f th narst stars t th cntr f th galaxy. This th analysis was mad n th basis f th systmatic bsrvatins by th Spac Tlscp "Hubbl" as m ч.д. 0,005 М гал. 4 г 9 кг (6) Th distanc ths stars frm th cntrs f th galaxis can b stimatd, if a gravity and a cntrifugal frc acting at th stars n thir rbits has bn balancd f mч. з. r pb () U 11 In ths frmulas, th gravitatinal cnstant f 6, N m / kg, m - mass f th 41 suprmassiv black hl at th cntr f th galaxy; M gal kg - th mass f th galaxy (th galactic nuclus); U-circumfrntial spd clsst t th cntr f th galaxy f th stars as thy mv in thir rbits. This a rat is stimatd by th amrican astrphysicist as 5. U km / hur 1,4 m / s. Fr ur th spiral galaxy Milky Way th rbital radii f narst t th cntr f th stars accrding t () will b , 1 15 r орб,4 м,4 км () 5 (1,4 ) Th radius f th suprmassiv black hl at th cntr f th Milky Way can b calculatd by th frmula () bcaus th phtns f a light can nt vrcm th gravity and lav th cr f th galaxy fmчд 1 9 rчд 1,49 м 1,49 км (9) C 9 Fr clarity, w lt us rmmbr that th radius f th rbit f th Saturn rrb 1,4 km. As yu can t s, th radius f th black hl cincids with th radius f th rbit f Saturn. This km.

4 prmptd th astrphysicists t suggst that in th cntr f th spiral galaxis thr ar th suprmassiv black hls which had dimnsins as th siz f th Slar systm. As yu can t s, th astrphysics hav awardd th massiv black hls in th cntrs f th spiral galaxis by a vry larg siz. At this siz, th avrag dnsity f th star turns ρ 0,01g / sm, which is a hundrd tims lss than th dnsity f a watr and nly tn tims gratr than th dnsity f th air at th surfac f th Earth. It must b rmmbrd that ths th stars can nt b sn and can nt b masurd. At th sam tim, th dnsity f th rdinary stars lik th Sun is f th rdr ρ 1,4 g / sm 1,4 kg / m, and th dnsity f whit dwarf stars cms t th valu f ρ hls. 9 0, g / sm. Th whit dwarfs is a visibl stars and nt th black Hr thr ar cnflict with th viws f th astrphysics. Indd, th black hls accrding t ths viws ar frmd du a cmprssin f a larg spars visibl stars and f a gas and a f dust cluds. Th dnsity f th black hls can nt b lwr than th dnsity f th whit dwarfs and prbably will tnd t valu f th dnsity f th nutrn stars. At this dnsity th rang f th radii f a suprmassiv black hl with th mass f th Milky Way wuld tak th valu mчд rчд 0,1 m 0km () ρ чд Accrding t th frmula (5) th cnditin fr th xistnc f a black hls in th thry f th gasus dark mattr can b writtn. This th cnditin dtrs th radii f th black hls frm th cnditin th inability t vrcm ncg radial flw dark gas by th wavs f a light. Fr th mass f th Milky Way, this frmula givs th fllwing valu f mчд r 1,15 m 1,15 km (11) α C It is in mr than n hundrd tims smallr than th radius f th black hl, dfind by (9). If th radius f a massiv black hl t tak in accrdanc with th thry f th gasus dark mattr (11), r 1,15 m 1,15 km thn th avrag dnsity f such a star is ρ 1,6 kg / m (1) This a valu is cls t th valu f th dnsity f th whit dwarf stars 1 ( 0,4 kg / m 0,9 kg / m ) and, thrfr it bttr is mt th mdrn astrphysics viws n th natur f a black hls. S, w hav th diffrnt stimats fr a dtring th radius f th suprmassiv black hl at th cntr f a spiral galaxy. On which n f thm t stay? It is 9 bvius that th assssmnt (9) r 1,49 km, is highr than th stimat f th thry f th gasus dark mattr r 1,15 km. This nly mans that th light frm any th surc in this ara can nt lav frm it. Th radius can nt b smallr than th radius f th suprmassiv stars () 0,1 km, bcaus th substanc can nt b cmprssd mr than th nutrn liquid r 4 1 with a dnsity ρ n kg / m suprmassiv black hl with a mass. Thus yu can with a crtainty b xpctd that th radius f a m 0, 005 M is in rang 4 0,1 km r 1,15 km (1) gal 4

5 9 Th radius r 1,49 km is t larg fr a black hl, bcaus this th rsult lads t th unralistically lw dnsity. Rcall that th basis f th all argumnts abut th suprmassiv black hls is th bsrvatinal fact, that in th cntrs f th spiral galaxis, astrnmrs can nt s th radiatin frm th lcal star. But thy saw that th circumfrntial spds f th stars clsst t th cntr is abnrmally high U km / h 140km / s. Withut this a cntral mass thy shuld b significantly lss. Th astrnmical bsrvatins suggst a dual rl f th galactic nucli. On th n hand th cntral suprmassiv black hls hav a vry grat gravity. This gravity can fully absrb th any clsly spacd stars r th thr matrial frmatin. In this rgard, th astrphysics mad th cnclusin that th black hls in th cntrs f a galaxis rprsnts a singularity. By dfinitin, this is th pint at which th substanc is disappars?? Eithr prmanntly r fr a tim?? Hw is it ging?? Whr ds it g??.th astrphysics can nt t xplain it. On th thr hand th thry f th gasus dark mattr rvals a scnd rl f th black hl. Indd, accrding t [1,] th dark mattr has th ability t a slf-rganiz, accmpanid by th phas transfrmatins f a gasus frms in a liquid frms and a slid frms. It is bsrvd n th Earth with a watr. A watr, as w knw, thr may b in th frm f a vapr, a liquid and a slid ic. In [] shwn that it bgins with dark mattr whn th vlcity f a jts f a gas dark mattr rachs valus f. U A,5 m / s. At th sam tim a larg amunts f a gasus dark mattr is changing t a small vlum f a dns liquid (slid) dark mattr. A liquid dark mattr acquirs th prprtis f a barynic mattr. it acquirs th prprtis f a gravity and an inrtia. Its dnsity 1 rachs th sam valu as that f th prtns and th nutrns ρ кг / м Th ur calculatins by frmula (4) shw that th rat at which a substanc crsss th surfac f th suprmassiv black hl with a radius r 1,15 km. is qual t V r α M 5,1 m/c (14) ρ r that is a littl lss than th maximum spd th jts f a dark gas V 5,196 m / c [1,]. Thus th scnd rl f th black hls is t crat a nw substanc frm th absrbnt dark mattr. This a matrial is jctd int th Univrs. Indd, th astrnmrs bsrvd th xpiratin f a hug masss f a nutral gas frm a galactic nucli. Thus suprmassiv th black hls ar a hug bilrs, in which was bing "brwd" a nw mattr frm th gas dark mattr and a nighbring stars that had bn absrbd bfr. This nw mattr thrwn int th vastnss t furthr its circulatin in th vast univrs. On th xampl f a whit dwarf stars and a nutrn pulsar, which was frmd as a rsult f th cllaps, i., as a rsult catastrphic cntractin f a mattr, it is xpctd that th suprmassiv black hls in th cntrs f th spiral galaxis, rtat vry quickly. It is clar that rsist a vry strng gravitatin can nly a cntrifugal frcs acting n th stars whn thy mv arund th galactic cntr. Th cntrifugal frcs ar in ur pinin may rsult t th missins f a mattr frm th cntr f th galaxy, if th cntrifugal frc xcds th frc f a gravity. max 5

6 W writ th cnditin f th dstructin f th black hl at th cntr f th galaxy. W bliv that th cntrifugal frcs sk t brak th suprmassiv star. Ths frcs ar balancd by th prssur frcs f th surrunding dark gas Fцб m чдω 1 (15) F r p p чд In this a cnditin, th paramtrs f th suprmassiv black hl: 6 9 m kg (th mass f a black hl in th cntr f th Milky Way). ω -is th angular vlcity f th rtatin. r - is th 5 radius f th black hl. 6,46 N / m -is th prssur in th gasus dark mattr [1,]. p W assum that th black hl at th cntr f th galaxy is lcatd within a sphr with a radius r 1,15 km dfind by th xprssin (11). Frm th rlatin (15) w btain th angular vlcity f rtatin f th suprmassiv black hl at th cntr f th Milky Way. If this spd was incrasd, th cntrifugal frcs xcd th prssur frcs and th star ar rlivd frm sm a mass r0чд p 1 ω 0,095c (16) m чд whr: r чд 1,15 m, prid f th rtatin π T 65, 6c ω 5 9 p 6,46 N / m, m чд kg In this cas, th circumfrntial spds n th stllar surfac -Black hls will U. This a valu crrspnds t th ω r,6 m c, (1) / This th vlcity xcds th spd f th light in a vacuum by.6 tims. D w nd t b afraid f it? Th thry f th rlativity frbids t mv at spds gratr than th spd f th light in th vacuum any a matrial bjcts. But w shuld nt frgt that th basis f such a ban is th pstulat f Einstin. This th pstulat is th thrtical th assumptins f th authr f rlativity thry. H bcam th dgma with an vr tim thanks t th ffrts f th rlativists. This th dgma has n th xprimntal cnfirmatin and has n th cnfirmatin f th astrnmical bsrvatins. Hnc it is nt th indisputabl truth. Mrvr, it suffics t slightly rduc th radius f th black hl bfr th valu r 0, m and t rduc th angular vlcity bfr th valu ω 0, 04 1/c. Rsulting th valu f th spd n th surfac black hl will hav qual t th spd f light. In this cas, th pstulat f th rlativity is nt vilatd. If th priphral spd and th angular vlcity is xcd th fund valus, thn th star shall t ls xcss a wight and t rduc thir th siz. W d nt knw whthr this will happn by an vlutinary way, r as a rsult f th xplsiv prcsss. If it happns in an vlutinary way, th jctd mattr wuld nt b abl t lav th ara, which dfind by th radius (9). This is bcaus, acting n it th cntrifugal frc ds nt vrcm th frcs f a gravity f a black hl. If thr is an xplsin f a star, thn thr will b an additinal radial vlcity. In this cas, w can t xpct that th jctd mattr will b xcd th spd f a light and shall lav th ara nar th black hl in th frm f a ht gass missins. Th suprmassiv black hl is vry tight frmatin having th sam dnsity as th whit dwarfs hav. Whn th liquid jts f a dark mattr fall n a dns surfac f th star thy can nt asily t pntrat thrugh th surfac f th star. Thrfr, th intractin f a liquid jts f a (1)

7 dark mattr with th stllar surfac will rsmbl th accrtin f a mattr. Lt us cnsidr th fllwing xampl. Lt th mass and th radius f th suprmassiv black hl is 9 M kg, r 1,15 m. Th jts f a liquid dark mattr is fall n th surfac f th star vry scnd and cntinuusly in th amunt f [1,]. α t α k M M M M ( 1) M t, (19) k whr M and M-ar masss stars at a givn mmnt f a tim and at th tim f th rigin. Th quantity f a mattr which is falling n th surfac f th whit dwarf at a spd α M Vr 5,1 m / s in pr unit tim will b qual ρ r α J M / t M 0,9 kg / s (0) k An nrgy ar supplid t th stllar surfac pr unit f a tim qual t th kintic nrgy f th mass flw 45 Q 0,5 J Vr 4 vt 4 rg / s (1) Th amunt f nrgy is accumulatd within 15 Gyr (4,5 1 s) insid a black hl (th black hl is nt radiats an nrgy) is LQ t4 45 4,5 1 1,9 6 эрг This an nrgy is nugh t slv th anthr riddl f th natur and t xplain th nrgy f th xplsin that is bsrvd in radi galaxis and in thr mystrius bjcts in th univrs. In this th xplsins is rlasd th nrmus nrgy simultanusly f th rdr f. Th astrnmrs ftn bsrv such th utbraks in th starry sky. Accrding t th mdrn astrphysics, such an nrgy can b rlasd nly whn th nuclar xplsin f all th stars f th whl galaxy ccurs simultanusly. This, f curs, is an incrdibl vnt, unlik frm th xplsin f n, albit f vry big th star. Such a star can b a suprmassiv black hl. Bibligraphy 1. Burag S.G. Gravity, dark, mattr and dark nrgy balanc. Th Gnral Scinc Jurnal. Astrphysics April. Papr ISSN pp. 0.. Burag S.G. Fundamntals f athrdynamics f Univrs. Hiddn sns f frmula E mc. Th Gnral Scinc Jurnal. Astrphysics. 01. April. Papr N441 6 pp.. Burag S.G. Athrdynamics - th ky t th mystris f th Univrs. Mscw: BkHus "Librkm", 009. pp ( (ISBN [in Russian]).