Collg Park, MD 011 PROCEEDINGS of th NPA 1 Gamma-Ray Lins of X-Class Solar Flar of July 3 rd, 00 Provid Dirct Evidnc for Nw Tird Light Lyndon Ashmor Dubai Collg, P.O. Box 37, Dubai, UAE -mail: wbmastr@lyndonashmor.com Th solar flar of July 3rd, 00 was th first ray flar to b obsrvd in high rsolution by th Ruvn Ramaty High Enrgy Solar Spctroscopic Imagr (RHESSI). Th obsrvations showd unxpctdly high rdshifts in th rays dtctd, but with no apparnt pattrn. Th shifts appar to b intrinsic as thy occur along a dirct lin of sight and not prpndicular to th solar surfac as xpctd by Dopplr ffcts. This papr looks at th wavlngths of th obsrvd photons and, in particular, th shift in ach wavlngth suffrd by th six nuclar d-xcitation lins of 1 C, 56 F, 4 Mg, 0 N, 16 O, 6 Si. What is found is that th data falls into two distinct sts. Each st has th shift in wavlngth dirctly proportional to th wavlngth as prdictd by Nw Tird Light (NTL). It is proposd that Si and F ar at diffrnt lvls in th solar atmosphr than th othrs and so photons from ths intractions travl shortr distancs through th solar plasma and thus undrgo smallr rdshifts. Thr also appars to b a quantisation in th shifts of th lins with fiv of th six lins showing shifts in wavlngths in multipls of.0 x 10-16 m. Ths rsults ar an anomaly in th mainstram xpansion thoris of rdshift but ar consistnt with th NTL thory. Hr, collision cross-sctions (and hnc shifts in wavlngth) ar proportional to th wavlngth of th photon and rdshifts ar causd by discrt shifts in wavlngth whn photons intract with lctrons in th plasma through which thy travl. That is, as th photons scap th solar plasma thy undrgo on, two, thr, four (and so on) intractions whr thy xprinc a shift in wavlngth of.0 x 10-16 m ach tim. Importantly, lin widths also provid dirct vidnc for NTL which prdicts that th lin widths should xprinc a statistical broadning that incrass as N - whr N is th numbr of intractions suffrd by th photons. For larg shifts in wavlngth th data shows a linar rlation btwn FWHM (Full lin Width at Half Maximum) and N as prdictd by NTL whr mainstram thoris prdict no variation. Ths rsults ar compard to th masurmnts of th solar flar of Octobr 003 and ar in good agrmnt. 1. Introduction As w will s latr, rdshift has a prcis mathmatical dfinition, but for now lt us just think of rdshift as photons of light/radiation having a longr wavlngth on arrival at th obsrvr whn compard with th obsrvr s standard of wavlngth for th sam lmnt with th ratio of th shift in wavlngth to th obsrvr s standard having th sam valu for a particular sourc. Thr ar svral known causs of rdshift such as gravitational rdshift (causd by photons gaining Gravitational potntial nrgy as thy climb a gravitational fild), or Dopplr rdshift causd by th sourc moving rlativ to th obsrvr. Thn thr ar th mor xotic thoris such as xpansion whr rdshift is causd by th photons bing strtchd as th spac thy ar travlling through xpands and strtchs thm; or Nw Tird Light (NTL) whr th photons los nrgy as thy travl through spac. Hr th photons ar constantly absorbd and r-mittd by th lctrons in th plasma of spac which rcoil at ach intraction. Th photons los nrgy to th rcoiling lctron, th frquncy of th photon rducs and th wavlngth incrass. It has bn rdshiftd. Thr ar svral rasons that mak th Solar flar of July 00 intrsting: Th gamma mission lins wr all cratd at approximatly th sam plac on th solar surfac and so should hav suffrd th sam Dopplr and gravitational rdshifts - and yt thy don t. Th rdshifts for ach lin ar diffrnt. If th rdshifts ar causd by xpansion ffcts thn again, sinc thy wr all cratd at th sam distanc from Earth, th intrvning spac would hav strtchd qually for all th gamma ray lins and so thy should all xhibit th sam rdshift. But thy don t, th rdshifts for ach lin ar diffrnt. In any cas, th distanc btwn th Sun and arth is not xpanding. Whn compard to th solar flar of 003, similar rsults in rdshift ar found and yt if ths rdshifts ar Dopplr ffcts thn thy should hav bn vry much diffrnt. Flars gnrally occur along magntic fild lins prpndicular to th solar surfac and so, with Dopplr ffcts, it is th componnt of vlocity towards Earth that would caus th rdshift. Sinc th Solar surfac is a sphr, flars at diffrnt positions on th surfac would hav diffrnt radial vlocitis towards th Earth and hnc a diffrnt rdshift. But thy don t. Th rdshifts of th lins ar similar rgardlss of th hliocntric angl - and so thy cannot b causd by Dopplr ffcts. It is as if th rdshifts ar causd intrinsically by th intrvning plasma as th photons travl dirctly towards us. This papr proposs that ths intrinsic rdshifts giv dirct vidnc for th NTL thory. So, thr ar svral rasons that mak th Solar flar of July 00 intrsting as it may giv us a tst to discriminat btwn
Ashmor: Solar Flar as Dirct Evidnc of Tird Light Vol. conflicting thoris. Th obsrvational rsults ar an anomaly in mainstram cosmology and yt thy ar just that - rpatabl rsults/obsrvations that must b xplaind. So lt us look at this in mor dtail. Smith t al [1] rportd th first high nrgy rsolution masurmnts of nuclar d-xcitation lins in th solar flar of July 3rd 00 using data from th Ruvn Ramaty High Enrgy Solar Spctroscopic Imagr (RHESSI) a spaccraft dsignd to obsrv th solar flars with high rsolution X ray and ray imaging spctroscopy. During solar flars, acclratd protons and alpha particls collid with th ambint nucli, xciting thm to a lvl abov thir ground stat. Gamma rays ar givn off during th subsqunt dcays as th nucli rturn to thir original lvl - thus crating th obsrvd nuclar d-xcitation lins. Sinc th nuclus rcoils both du to th intraction with th acclratd particls and du to th mission of th rays, th lins can b Dopplr shiftd. Howvr, Smith t al [1] found that th masurd rdshifts wr much largr than xpctd from ths Dopplr mchanisms alon. Possibl xplanations put forward wr ithr that th magntic fild lins ar dirctd towards th Earth rathr than bing prpndicular to th solar surfac or that th angular distribution of th intracting particls is closr to a forward bam than a forward isotropic distribution.. Shift in th Wavlngth of th Lins Isotop Rst Enrgy (kv) Fit Enrgy (kv) 56F 47 0.70 46.09 0.60 4Mg 1369.3 1363.0 0N 1634 1.7 16 1.7 Si 1779 1.9 1776.1 1C 443 10 4403 10 16O 619 15 6094 1 Tabl 1. Paramtrs of Nuclar Lins % Rdshift 0.0 0.11 0.07 17 0.40 0.14 0.10 0.3 0.10 0.11 0.1 0.1 0.3 0.79 0. 0.4 0.5 0.9 Th dtctors on RHESSI masur th nrgis of th incoming gamma rays but it is th wavlngths and in particular th shifts in wavlngths that ar of importanc in thoris on rdshift. (Tabl ). Isotop Rst λ /10-13 m Obsrvd λ /10-13 m 56F 14.64 0.0010 14.6639 0.001 4Mg 9.0971 0.01337 9.0971 0.0153 0N 7.5930 0.00795 7.6177 0.00795 Si 6.97414 0.006 6.97 0.00746 1C.79563 0.0064.175 0.0063 16O.0431 0.06030.03594 0.00500 Shift in wavlngth Δλ/10-16 m Priodicity in shifts of.0/10-16 m.6 4.0 4.3 4.0 6 1 3.0 5 6.0.5 10 16 1 5.0.0 6.0 7 4.0 6 11.0 3.0 4 4.0 1.0 4.0 13 36 15 6.5 1.0 7.5 Tabl. Paramtrs of Nuclar Lins in trms of wavlngth Th rdshift z is a scintific trm dfind as: z (1) Th lins giv startling vidnc of quantisd shifts in wavlngth. A quantisation of.0x10-16 m givs a good fit with fiv of th six lins giving prcis quantisation whilst th sixth ( Si) is vry clos and wll within th confins of th uncrtaintis. Howvr, th quantisation is clos to th prcision of th data and w must worry in cas ths ar rounding rrors. Thr is a 50/50 chanc of th numbrs bing vn or odd and th chancs of gtting fiv out of six vn numbrs ar approximatly on in tn and ar thus not significant at th 5% lvl. 3. Obsrvation of th Solar Flar of Octobr th, 003 On Octobr th, 003 occurrd th scond most powrful flar vr obsrvd up to that point by SOHO (Solar and Hliosphric Obsrvatory) and this flar was dtctd by th SPI and IBIS dtctors on board th spaccraft INTEGRAL (Europan Spac Agncy s gamma, X-Ray and visibl obsrvational satllit) []. Masurmnts of th nuclar d-xcitation lins producd in this solar flar nabld th rdshift in two of th lins ( 16 O and 1 C) to b dtrmind and so w can compar ths rsults with thos from th RHESSI for th July 00 flar. Th hliocntric angl is shown in Tabl 3. hl Rst Enrgy % rdshift % rdshift (kv) 003 flar 00 flar hl 30 0 73 0 443.03 ( 1 C) 0.097 0.63 0.097 61.63 ( 16 O) 0.1 0.59 0.1 0.3 0.79 0. 0.4 0.5 0.9 Tabl 3. Comparison in wavlngth shifts for th two flars Isotop Shift in λ 00/10-16 m Shift in λ 003/10-16 m 1C 7.7 6 17..7 16O 6 1 9.5 5 11.9 9.5 Tabl 4. Paramtrs of th Oxygn and Carbon lins in 00 and 003 flars It can b sn that whilst th rdshifts for th 16 O lin is th sam for both flars, thr is quit a diffrnc in th masurd rdshifts of th 1 C lin. Could it b that th Carbon lmnt in th 00 flar was lowr in th solar atmosphr than that in 003 and thus suffrd a gratr rdshift as pr th NTL Thory? It should b notd that th rsults for th two flars ar similar rgardlss of th hliocntric angl - which is in disagrmnt with thortical modlling of th lins that prdict that th shifts should incras as hliocntric angl incrass. Again, ths masurmnts ar in trms of photon nrgy and so to s if th sam quantisation ffcts ar prsnt in th 003 flar w nd to convrt to shifts in wavlngth (Tabl 4). W now hav a total of svn out of ight shifts in wavlngth which ar vn (a probability of on in thirty two, or approximatly 3%). This is significant at th 5% confidnc lvl.
Collg Park, MD 011 PROCEEDINGS of th NPA 3 Th shift in th 16 O lins ar consistnt in both flars at a quantisation of 6x(.0x10-16 m) - as bfor. Howvr, whilst thr is a significant diffrnc btwn th nrgis and rdshifts of th obsrvd 1 C lins, th pattrn of quantisation in th shift of wavlngths continus with a priodicity of.0x10-16 m. Th shift in th 1 C lin in 00 bing 11x(.0x10-16 m) whilst that in 003 bing 9x(.0x10-16 m). 4. Intrinsic Hubbl Law As has bn statd arlir, thr should b no cosmological ffcts on ths gamma ray lins and any Dopplr ffcts would b ngligibl compard to thos dtctd. Thus any rdshifts must b producd intrinsically by th solar plasma. That raiss th qustion, do th intrinsic rdshifts oby th Hubbl Law? To oby th Hubbl Law, on of th critria is that a graph of shift in wavlngth vrsus wavlngth should b a straight lin through th origin. Thus th rdshift, z is th sam for all wavlngths. Th data falls into two distinct sts with O, 3 C, N and Mg forming on st with z 4.3x10 and Si and F 3 forming th othr st with z 1.x10. Th data is consistnt with intrinsic rdshifts providd that w assum that Si and F ar highr in th solar atmosphr. Th photons of th nuclar d-xcitation lins of ths two lmnts travl a shortr distanc through th plasma, mak fwr photonlctron intractions on thir way to th Earth and thus xprinc a smallr shift in wavlngth. Howvr, in both cass, th shift in wavlngth is proportional to th wavlngth - as rquird by th Hubbl law. Fig. 1. Shift in Wavlngth vrsus Wavlngth It must b rmmbrd that th Big bang/xpansion thory prdicts no rdshift in ths lins at all. Mainstram Physics can offr no xplanation for this phnomnon. NTL thory prdicts a rdshift in ths lins and prdicts that th shift in wavlngth is gratr for longr wavlngths sinc th collision cross-sction, σ for photon-lctron intractions is givn by: r. 5. Lin Widths and Nw Tird Light Anothr way to discriminat btwn th NTL and th Big Bang modls using this data is in th lin widths [3]. Normally th Dopplr paramtr (b) is usd as a masur of lin widths. Th Dopplr Paramtr (b) is rlatd to th tmpratur and dgr of disturbanc of th mitting or absorbing gas by: b = b th + b nt wr b th and b nt ar th thrmal and non thrmal broadning of th lin. Sinc all th lins in th solar flars wr mittd from approximatly th sam plac w would xpct th Dopplr broadning to b th sam for all mission lins (assuming lmnts at th sam plac on th solar surfac to b in thrmal quilibrium). Th Big Bang modl prdicts no chang in th lin width of ths lins with rlation to wavlngth. With th NTL thory, th lins broadn du to statistical fluctuations in th numbr of intractions N ncountrd btwn photon and lctrons in th plasma of spac. Th standard dviation in th numbr of intractions and hnc lin width should incras with distanc and rdshift - as th squar root of N to b prcis i.. th gratr th numbr of intractions th widr th lin. whr thrmal lin broadning and tot th N tot is th total standard dviation du to statistical and is that du to thrmal ffcts th alon. It can b sn from Fig that for valus of N lss than 3., th FWHM is similar for all points. It is proposd that in this rgion th ffcts of statistical lin broadning du to th NTL thory ar not significant whn compard to lin broadning du to thrmal and or th dgr of disturbanc. Howvr, for valus of N abov 3. thr is a linar rlation btwn FWHM and N as prdictd by NTL. That is, th longr th wavlngth of th photons, th mor collisions thy mak, th gratr th shift in wavlngth and th gratr th standard dviation in th numbr of collisions. Sinc ach photon-lctron intraction rsults in a quantisd incras in wavlngth th lins broadn as N. In th Big Bang/xpansion thory, thr should b no diffrnc in th lin broadning - rgardlss of wavlngth. Sinc th photons wr producd at th sam distanc from Earth and at th sam plac and sam tim, thy should all suffr th sam Dopplr lin broadning. It is clar that thy don t and thus th lin broadning in this solar vnt of 00 givs dirct vidnc in favour of Nw Tird Light and against xpansion. On could ask th qustion at this point Why don t th lins usd to dtrmin rdshifts of distant galaxis broadn as th rdshift incrass? Th answr to this is in two parts as w must trat mission lins and absorption lins sparatly. Absorption lins ar an absnc of photons and so on would not xpct an absnc of lins to broadn. What happns is th continuum broadns into th absorption lins making thm narrow with incrasd rdshift. A study of th litratur on th Lyman Forst shows just this. Th Lyman absorption lins for narby Hydrogn clouds ar, on avrag, broadr than thos from clouds at gratr rdshift in fact thr is a gnral trnd of th absorption lins narrowing in th data z = 0.1 up to z = 3.6 [3]. Emission lin widths ar mor complx as NTL dos prdict that ths will broadn. An mission lin from a galaxy twic as far away will travl twic as far through th plasma of intrgalactic spac, mak twic as many collisions and thus th standard dviation will incras by a factor of. Howvr, sinc th galaxy is twic as far away it will b dimmd by a factor of four du to th invrs squar law, and thus w must collct mor photons from that lin (four tims as many) - in ordr to mak th xposur.
4 Sinc w hav an initial sampl siz incrasd by a factor of four, th initial standard dviation of our sampl is now only half ( 1 N ) as wid as that of th closr galaxy. It is proposd that th ffct of using a largr initial sampl siz from a mor distant (dimmr) galaxy (and thus a smallr standard dviation to bgin with) masks th lin broadning du to NTL. This is to b th subjct of a futur papr - not rady at th tim of going to prss. Fig. FWHM vrsus 6. Nw Tird Light Rvisitd In ordr to s th importanc of ths rsults w nd to rvisit th NTL thory [4]. Elctrons in th plasma of IG spac (or any plasma for that mattr) can prform SHM and any lctron that can prform SHM can absorb and rmit photons of light. [5,6]. To quot, Th lctron just has a natural oscillation frquncy qual to th local plasma frquncy, and w gt a simpl pictur of rsonanc absorption in trms of th driving fild bing in rsonanc with this natural frquncy. [7]. Th plasma in IG spac is known to hav a frquncy of lss than 30Hz [] and so th driving fild i.. th photon of light, has a driving frquncy far abov rsonanc. In consqunc, rsonanc absorption will not tak plac and th photon will always b r-mittd. In th sparsly populatd plasma of intrgalactic spac th lctron will not only absorb and rmit th photon but will rcoil ach tim. Th nrgy lost to th rcoiling absorbing/mitting systm is wll known [9] and givn by: Enrgy lost to an lctron during mission or absorption = Q /m c, whr Q is th nrgy of th incoming photon, m th rst mass of th lctron and c th spd of light. This must b applid twic for absorption and rmission. Hnc, total nrgy lost by photon = Q / m c h c / m (nrgy bfor intraction) (nrgy aftr) = Ashmor: Solar Flar as Dirct Evidnc of Tird Light Vol. N hc / hc / h / m hc / m (4) = initial wavlngth of photon, = wavlngth of th rmittd photon. Multiplying through by m and dividing by h, givs: mc mc h Incras in wavlngth, so: => (5) ( ) mc mc h( ) (6) mc mc mc h h (7) => sinc h m c mch h () h/ m c (9) On thir journy through IG spac, th photons will mak many such collisions and undrgo an incras in wavlngth of h/ m c ach tim. On this basis rd shift bcoms a distanc indicator and th distanc - rd shift rlation bcoms: photons of light from galaxis twic as far away will travl twic as far through th IG mdium, mak twic as many collisions and thus undrgo twic th rd shift. Consrvation of linar momntum will nsur th linar propagation of light. 7. Th Hubbl Law Th procss whrby a photon intracts with an lctron and givs all its nrgy to th lctron is known as photoabsorption and th photoabsorption cross sction, σ, is known from th intraction of low-nrgy x rays with mattr [10,11,1]. r f (10) whr r is th classical radius of th lctron and f is on of two smi-mpirical atomic scattring factors dpnding, amongst othr things, on th numbr of lctrons in th atom. For 10 kv to 30 kv X-rays intracting with Hydrogn, f has valus approximatly btwn 0 and 1. On maning that th photon has bn absorbd and th atom rmaining in an xcitd stat and zro maning that th photon was absorbd and an idntical photon rmittd [13]. Collision cross sctions hav th units of ara and rprsnt a probability that th intraction will tak plac. In a photonlctron intraction thr ar only two possibl outcoms. Eithr th photon is absorbd and not r-mittd (rsonanc absorption, f = 1, and probability of r-mission = 0) or th photon is absorbd and a nw photon is mittd (transmission, f = 0 and probability of r-mission = 1). Consquntly whn th photon frquncy is wll off rsonanc th probability of absorption is zro and th probability of r-mission is on. For conditional probability wr w nd th photon absorbd AND r-mittd, r is th probability of absorption and f is th probability of r-mission, and so w multiply th two sparat probabilitis. Sinc f has th valu of unity th collision cross-sction for transmission is r. Th atomic scattring factor, f, only modulats th collision cross-sction r and so this is th trm w nd. Elctrons in plasma bhav in th sam way as thos in an atom. Sinc th photon frquncy of light from distant galaxis is far rmovd from th rsonant frquncy of th lctrons in th plasma of IG spac, th photons will always b rmittd. On thir journy through th IG mdium, photons of radiation at th rd nd of th spctrum will ncountr mor collisions than photons at th blu nd of th spctrum and thus undrgo a gratr total shift in wavlngth. For a particular sourc, th ratio will b constant. For larg distancs or a larg numbr of intractions, th collision cross-sction incrass as th photons ar rdshiftd and this lads to an xponntial Hubbl diagram and th prdiction of
Collg Park, MD 011 PROCEEDINGS of th NPA 5 ffcts usually put down to acclration. Howvr, for ths solar flars it is a good approximation to assum that it is constant as th prcntag rdshifts ar small. W hav r. Th man fr path is givn by n 1 or nrd 1 whr n is th man lctron dnsity. Th total numbr of intractions, N, suffrd by th photon in travling a distanc, d, is simply th distanc dividd by th man fr path. d N nr or N n r d 1 Th total shift in wavlngth suffrd by th photon, N and sinc rdshift z is givn by z / w hav:, is nhr z mc W hav v cz and v Hd whr v is a trm attributd to vlocity in th Big Bang thory and H is th Hubbl constant. This lads to an xprssion for H as: nhr H m Publishd valus of th Hubbl constant ar around H = 64±3 km/s pr Mpc or, in SI units,.1x10-1 s -1. An stimatd valu of n in th IG spac can b achivd from th WMAP data [14] and givs n =.x10-7 cm -3 or an avrag of 0. lctrons pr mtr cubd. Thus this NTL givs a prdictd valu of H as 0.9x10-1 s -1 or 7 km/s pr Mpc. Thus th thory s prdictd valu of H from first principls is in good agrmnt with th obsrvational valu. Howvr, it should b notd that in th solar flars n and th ffctiv mass m ar much diffrnt than IG spac. It should b notd that rdshifts hav now bn inducd in cold plasma in th laboratory. A pulsd lasr was fird at a crystal producing plasma and th wavlngth of th rcombination lins masurd. Thy wr sn to b rdshiftd with th dgr of rdshift incrasing with plasma fr lctron dnsity [15]. Thr is thus vidnc from th laboratory that cold plasma inducs rdshifts and thrfor givs support to th NTL thory.. Cosmic Microwav Background (CMB) Whilst not of particular intrst to us hr with rgard to th solar flars, NTL also prdicts th CMB. Th rcoiling lctron will b brought to rst by Coulomb intractions with all th lctrons containd within a Dby sphr of radius λ D. Th dclrating lctron will mit transmission radiation (TR) i.. brmstrahlung. Thr ar two mission channls of th systm, intrinsic mission by th dclrating lctron, and mission by th mdium whr th background lctrons radiat nrgy. Th intractions btwn light and th lctrons ar nonrlativistic and th initial and final stats of th lctron blong to th continuous spctrum. Th photon frquncy of th transmission radiation f cmb is givn by: cmb 1/ hf m p p (4) whr p mv and p mv ar th initial and final momntum of th lctron [15]. Th lctron rturns to rst aftr absorption and rmission and so th wavlngth of th transmission radiation λ cmb is givn by: cmb m c/ h (5) Light of wavlngth 5x10-7 m givs ris to TR of wavlngth 0.1m. In IG spac, th dominant background photons ar microwavs, having pak nrgy of 6x10-4 V and a photon dnsity of about 400 pr cm -3 [16,17]. In this thory, ths background photons (λ =.1x10-3 m) would b givn off as TR by a photon of wavlngth 5x10 - m (i.. Ultra Violt radiation) intracting with an lctron. Intrstingly, th CMB has a black body form of radiation and it is known that plasma mit Black Body radiation as th clouds will b in thrmal quilibrium. To quot, whn vry mission is balancd by an absorption by th sam physical procss this is th principl of dtaild balanc. Th radiation spctrum must hav a black body form in thrmodynamic quilibrium. That is whn th mission of a photon is du to th absorption of a photon, th mission will b black body [1]. Thr is good vidnc for plasma bing rsponsibl for rdshifts in IG spac as intrinsic rdshifts hav bn rcratd in th laboratory within lasr inducd plasma with th dgr of rdshift incrasing with fr lctron dnsity [19]. 9. Discussion W s that th NTL thory prdicts a quantisd rdshift of hmc on ach photon lctron intraction whr m is th ffctiv mass of th lctron. In IG spac whr th plasma is vry spars m has th valu clos to th rst mass of th lctron. Howvr, as th plasma incrass in dnsity, lctrostatic forcs btwn th ions incras th ffctiv mass of th lctron and so th quantisd shift in wavlngth on ach intraction dcrass. This is why w obsrv no rdshift whn light travls through glass. Th lctrons ar bound in atoms which ar bound in th block of glass. Just as in th Mössbaur ffct, th ffctiv mass bcoms th mass of th block of glass and no rcoil taks plac and thus no nrgy is lost by th photons. Th plasma around th Sun is dnsr than that in IG spac but not too dns so as to prvnt rdshifts taking plac. Howvr, th quantisd shift on ach intraction will b lss and thus th rsults of both flars ar consistnt with NTL but not th BB thory. All lins support a quantization in shifts in wavlngth of.0x10-16 m. Intrstingly, whilst th 1C lins of 00 and 003 diffr in thir rdshifts and actual shifts in wavlngth, th two rsults still dmonstrat th quantisation pattrn with th 003 rsult showing a priodicity of lvn whilst th 003 rsult shows a priodicity of nin. Th rdshifts in th gamma mission lins giv dirct vidnc for th NTL thory not only in thir quantisation. Th rdshifts ar too big to b du to any mainstram proprty (Dopplr, gravitational, xpansion) and act in a dirction on a dirct lin of sight. Th rdshifts ar intrinsic and w s that thy oby th ssntial proprty that th shift in wavlngth is dirctly proportional to th actual wavlngth in ordr to comply with th Hubbl law. Nw Tird Light xplains sinc collision cross sctions ar proportional to th wavlngth of th photon. A photon with twic th wavlngth maks twic as many collisions in travling
6 Ashmor: Solar Flar as Dirct Evidnc of Tird Light Vol. th sam distanc and thus undrgos twic th shift in wavlngth. Th data falls into two sts with ach st forming thir 3 3 own valu for th rdshift z. ( z 4.3x10 and 1.x10 ). Again, this is inconsistnt with th Big Bang thory but consistnt with NTL which xplains th data sts as bing du to th lmnts bing at two diffrnt hights in th solar plasma. O, C, N and Mg bing lowst and thus ths photons travl furthst through th plasma and undrgo gratr shifts in wavlngth than thos producd by Si and F. Isotop Si (00) 16O (00) 6 5 Shift in λ Δλ/10-16 m 16O (003) 11.9 9.5 9.5 56F(00) 10 16 1 1C(00) 7 6 1C(003) 17..7.7 0N(00) 4Mg(00) 13 36 15.6 4.0 4.3 4.0 1 3.0 6.0.5 Priodicity in th shifts of /10-16 m 4.7 5. 4. 5.0.0 6.0 4.0 11.0 3.0 1.4.9 1.4 4 4.0 1.0 4.0 6.5 1.0 7.5 Tabl 5. Priodicity in rdshift for all data Of particular importanc is th lin widths. In th Big Bang Thory, Dopplr tc th shift in wavlngth should not affct th lin width but it dos. For lins undrgoing larg shifts in wavlngth thr is a linar rlationship btwn and N as prdictd by NTL. This is clar, dirct vidnc for Nw Tird Light. 10. Conclusion Ths solar flars form an nigma in mainstram astrophysics as thy produc rdshifts which cannot b xplaind. Howvr, thy provid dirct vidnc in favour of Nw Tird Light. Th flars giv vidnc of quantisation in th shifts of wavlngth as prdictd by Nw Tird Light but not by mainstram thoris. Th rdshifts appar to b intrinsic sinc thy occur along a lin of sight and not prpndicular to th solar surfac. Th intrinsic shifts in wavlngth ar proportional to th actual wav lngth as prdictd by Nw Tird Light vn though th data falls into two distinct data sts. Th Big Bang Thory and othr mainstram thoris do not prdict a link btwn lin width (FWHM) and shift in wav lngth. Nw Tird Light prdicts FWHM valus to b dirctly proportional to N. For larg shifts in wavlngth this data shows thr is a linar rlationship btwn th two and thus supports Nw Tird light ovr othr thoris. To ths rsults w must add th prvious succsss of Nw Tird Light such as succssfully prdicting th Hubbl Law and valu of th Hubbl constant and th CMB. Acknowldgmnt I would lik to thank John Kirnan for bringing th papr High-Rsolution Spctroscopy of Gamma-Ray Lins from th X-Class Solar Flar of 00 July 3 by Smith t al [1] to my attntion. Rfrncs [ 1 ] D. M. Smith t al, ApJ 595: L1-L4 (003). [ ] M. Gros t al, INTEGRAL/SPI Obsrvation of th 003 Oct Solar Flar, http://www.mp.mpg.d-gamma-instrumntsintgral.spi-www-paprs-solflar0310_gros_iwso4.pdf.url. [ 3 ] L. E. Ashmor, Hydrogn Cloud Sparation as Dirct Evidnc of th Dynamics of th Univrs, in Frank Pottr, Ed., ASP Confrnc Sris 413: 3 (nd Crisis in Cosmology Confrnc, CCC-, 009) http://adsabs.harvard.du/abs/009aspc..413...3a. [ 4 ] L. E. Ashmor, Galilan Elctrodynamics 17 (S3): 53-57 (006). [ 5 ] M. Mitchnr, C. H. Krugr, Partially Ionizd Gass, p. 13 (Wily, 1973). [ 6 ] W. S. Kurth, Wavs in Spac Plasmas, http://www-pw.physics. uiowa.du/plasma-wav/tutorial/wavs.html. [ 7 ] R. A. Cairns t al, Physica Scripta T75: 99-103 (199). [ ] M. V. Zombck, Handbook of Spac Astronomy and Astrophysics, p. 6 (Cam Uni. Prss, 010), http://ads.harvard.du/books/ hsaa/idx.html. [ 9 ] A. P. Frnch, Spcial Rlativity, p 176-1 (London: Nlson, 196). [ 10 ] B. L. Hnk, E. M. Gullikson, J. C. Davis, Atomic Data and Nuclar Data Tabls, Vol. 54, pp. 11-34 (1993). [ 11 ] B. L. Hnk, E. M. Gullikson, J. C. Davis, X-Ray Data Booklt, chap 1, p 44/5 (LBNL/PUB-490 Rv. Lawrnc Brkly National Laboratory, Univrsity of California, Brkly, CA 9470, 001) http://www-cxro.lbl.gov/optical_constants/intro.html. [ 1 ] J. H. Hubbll, W. J. Vigl, E. A. Briggs, R. T. Brown, D. T. Cromr, R. J. Howrton, J. Phys. Chm. Rf. Data 4: 471-53 (1975); rratum in 6: 615-616 (1977). [ 6 ] A. P. Frnch, Spcial Rlativity, p 1 (London: Nlson, 196). [ 13 ] F. Zwicky, Proc. Nat. Acad. Sci. 773 75 (199). [ 14 ] A. M. Soltan, A&A 40: 39-4 (003). [ 15 ] K. Yu. Platonov, G. D. Flĭshman, Uspkhi Fizichskikh Nauk 17 (3) 41-300 (00). [ 15 ] V. B. Brsttskii, E. M. Lifshitz, L. P. Pitavskii, Quantum Elctrodynamics, Vol. 4, nd Ed., p. 39 (Buttrworth Hinmann, 19). [ 16 ] P. J. E. Pbls t al, Th cas for th rlativistic hot Big Bang cosmology, Natur 35: 769-776 (9 Aug 1991), doi:10.103/35769a0. [ 17 ] M. Nagano & A. A. Watson, Rviws of Modrn Physics 7 (3): 69-73 (July 000). [ 1 ] M. S. Longair, High Enrgy Astrophysics, Vol. 1, nd Ed. (Cambridg Univrsity Prss, 191). [ 19 ] C. S. Chn t al, Invstigation of th mchanism of spctral mission and rdshifts of atomic lin in lasr-inducd plasmas. Optik 10: 473-47 (009).