Baryon number from collapsing cosmic strings

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<ul><li><p>Volume 119B, number 1,2,3 PHYSICS LETTERS 16 December 1982 </p><p>BARYON NUMBER FROM COLLAPSING COSMIC STRINGS </p><p>P. BHATTACHARJEE, T.W.B. KIBBLE and Neil TUROK Blackett Laboratory, Imperial College, London SW7 2BZ, England </p><p>Received 14 July 1982 </p><p>In those grand unified theories that predict the existence of stable strings, closed loops may be formed and collapse, releasing their energy in the form of particles. We point out that this process may be an important contributor to the net baryon number of the universe. </p><p>The occurrence of topologically stable strings in some grand unified theories may be a positive feature. As pointed out by Zel'dovich [1], strings formed at the grand unification phase transition could later provide the density perturbations necessary to "seed" the pro- cess of galaxy formation. Vilenkin [2] has proposed a more realistic scenario relying on stable loops formed by self-intersection of strings rather than on very long strings. This idea has been strengthened by the dis- covery by two of us [3] of a class of stable spinning loop solutions. We also showed that any initially static loop collapses to a point or, more generally, a doubled loop * 1 (a configuration in which the string winds twice round the same loop) after a time L/4, where L is its initial length (and c = 1). Z 2 strings would then presumably annihilate into particles. Z 3 strings might "add" to form a string in the opposite direction with some release of particles. For other strings yet more complex processes could occur. We also showed that the lowest frequency mode non-static loop collapsed to a line at t </p></li><li><p>Volume 119B, number 1,2,3 PHYSICS LETTERS 16 December 1982 </p><p>formed in two ways - either when already existing loops enter the horizon, or by the self-intersection of longer strings. It is not at all clear what fraction of these may be formed in initially static or near-static configurations or in other collapsing configurations, but here we shall make what seems to be a not unrea- sonable assumption that the fraction is significant. These loops will then collapse to a doubled loop, a line or in special cases a point. These last will form black holes, while the others (at least in the case of Z 2 strings) annihilate and release their constituent boson quanta, both gauge bosons and Higgs particles. A rough estimate of the number of superheavy bosons released per unit invariant length of string is simply la/m X. </p><p>As argued by Vilenkin [2], a consistent picture re- quires that the increase in string energy due to confor- mal stretching of long strings (i.e. strings extending be- yond the horizon) must be compensated by some mechanism of energy loss. He takes this to be the pro- cess of loop formation and collapse. If so, the rate of creation of loops per unit volume is </p><p>dn/dt ~ 1/t 4 . </p><p>A typical loop created at time t has a radius of order t [2] and therefore collapses, as explained above, at or before a time t(1 + 3,/4) where ~'t is its length (7 ~ 2rr). If it collapses to a doubled loop it gives rise to a net baryon number of order eTtu/mx, where e is the mean net baryon number produced in the decay of a super- heavy boson. </p><p>We can now estimate the total baryon asymmetry produced by all loops collapsing after the damping period. The entropy density is </p><p>s = ~ ~r2NT 3 ,'~ 50 T 3 . </p><p>During the expansion the ratio nB/s is constant except for the contribution from collapsing loops (or other baryon-number-generating processes). Since the num- ber of bosons decaying is small compared to the num- ber of particles already present, their contribution to the entropy is negligible. Hence </p><p>(d/dt) (nB/s) = (I/s) (dnB/dt)loops. </p><p>Integrating from t = t e onwards (effectively to ~) we find </p><p>(n B/s)fina 1 ~ 300 fep 2 /m X m3p </p><p>300 (fe/~ 2 ) (mx /mp) 3 , </p><p>where f i s the fraction of loops produced that collapse in this way. If f is of order 10 -1 andm X ~ 5 X 1014 GeV, we get typically nB/s ~ 10 -8 e. </p><p>If, following Nanopoulos and Weinberg [6], we as- sume that e lies in the range between 10-2 and 1, we obtain a value in good agreement with the present ob- servational bound n B/s ~ 10- 9.8 +- 1.7 [7]. </p><p>This is of course in addition to any baryon asymme- try created earlier. One interesting feature of the mechanism is that baryon number is not generated uni- formly throughout space but in clumps around the col- lapsing strings. However the scale of these clumps is too small to be of any relevance to galaxy formation. </p><p>Great uncertainties remain in this theoretical predic- tion. First, the number of superheavy bosons released per unit length of collapsing string is uncertain. It should be possible to calculate it, but a deeper under- standing of the quantum or at least semiclassical theory of strings is needed. Second, the estimate of the time t e at which the process of baryon-number genera- tion by collapsing strings effectively begins is rather crude. In reality there is no sharp beginning. The pro- cess is a continuous one. Numerical calculations are presently under way to improve this estimate. But since nB/s ~x te 1/2, we do not expect the result to change very significantly. Lastly, the parameter e is highly model-dependent and cannot at present be cal- culated from first principles. </p><p>What we have shown however is that this process of collapsing cosmic strings may be a signficant contri- butor to the total net baryon number of the universe. Certainly in those GUTs that predict the appearance of stable strings it cannot be ignored. </p><p>One of us (PB) would like to thank The Royal Com- mission for the Exhibition of 1851, London, England for financial support. </p><p>References </p><p>[1] Ya. B. Zel'dovich, Mon. Not. Astron. Soc. 192 (1980) 663. </p><p>[2] A. Vilenkin, Phys. Rev. Lett. 46 (1981) 17. [3] T.W.B. Kibble and N. Turok, Phys. Lett. l16B (1982) 141. [4] T.W.B. Kibble, J. Phys. A9 (1976) 1387. [5] A.E. Everett, Phys. Rev. D24 (1981) 858. [6] D.V. Nanopoulos and S. Weinberg, Phys. Rev. D20 (1979) </p><p>2484. [7] G. Steigman, Ann. Rev. Astron. Astrophys. 14 (1976) </p><p>339. </p><p>96 </p></li></ul>