Dark Matter Does not Exist at all

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1 Journal Heading Year; Vol. (No.): page range DOI: /j.xxx.xxxxxxxx.xx Dark Matter Does not Exist at all Mario Everaldo de Souza 1 /1 Departamento de Físia, Universidade Federal de Sergipe, São Cristovão, , Brazil Abstrat Several aspets of the dark matter proposal are disussed. It is shown that the existing baryoni mass in galaxies is suffiient for losing the Universe. It is onluded, then, that dark matter does not exist at all in the Universe. Keywords Dark matter, WIMPs, Closed Universe, Peuliar veloities of galaxies 1. Introdution It has been proposed by many researhers [1,,3,4] that a mysterious kind of matter, alled dark matter, exists inside galaxies and also in the spae among galaxies. Aording to its proponents dark matter would have an important role in the dynamis of spiral galaxies [4], in the dynamis of galaxy lusters [3,5], in galaxy formation [6], in the large-sale-struture formation [6], and would provide 6.8% for the mass of the Universe in order to have a losed Universe, aording to the Standard Cosmologial Model, the soalled Lambda-CDM [7]. These seven referenes in this paragraph are just examples of a vast literature on the subjet and some of these are pioneering artiles. Dark matter would have very unusual properties as it would not suffer the eletromagneti interation, and would be, thus, ompletely invisible. It is supposed existene would be inferred only from its gravitational effets in galaxies and galaxy lusters. This means that it would have to be extremely stable. It would be omposed of weakly interating massive partiles (WIMPS) that would interat only through gravity and the weak interation. This means that WIMPS would have to be very speial heavy fermions beause they would be ompletely stable and neutral. *Corresponding author: mariodesouza.ufs@gmail.om Other researhers have proposed that WIMPS ould be omposed of axions [8]. This partile is a hypothetial elementary partile postulated within the framework of the Peei-Quinn Theory [9,10]. Currently there are the proposals of Kim- Shifman-Vainshtein-Zakharov [11,1] and of Dine-Fishler-Sredniki-Zhitnitsky [13,14]. My ritiism in this ase is that the axion is a spin 0 boson and matter is omposed of fermions, suh as atoms, nulei, nuleons. Bosons take part in matter intermediating fermioni states. Thus, it does not make any sense to onsider a large volume of bosons. And there is an additional serious drawbak: All bosons with mass are unstable.. Leptoni WIMPs Have no Plae in Partile Physis Any matter is omposed of partiles and this should hold for dark matter, of ourse. As disussed above, leptoni WIMPS would have to be very stable neutral leptons. This means that there would be another family of speial leptons, and this would ause a hange in the symmetry of the Weinberg-Salam eletroweak theory whih is a very preise theory. As above disussed dark matter partiles would have to be very heavy leptons, but a basi fat of Partile Physis is that the heavier a partile is, the more unstable it is. It is hard to figure out where the WIMP would fit in the table of leptons below. In the table below the muon and the tau are unstable, and, thus, only the lightest lepton (with proven mass) is stable.

2 author name (et al.): artile title Table 1. The leptons of Nature 5. The Lambda-CDM Cosmologial Model Has too many Flaws e e e e Kroupa [17] raises many important issues on the existene of dark matter and shows that the so-alled Lambda-CDM osmologial model has too many flaws and thus does not desribe reality at all. 6. Reent null Results of Dark Matter It is also very important to have in mind that all neutral partiles (not leptons, of ourse) with mass are omposed of harged onstituents and, thus, all neutral partiles with mass interat by means of the eletromagneti interation. Therefore, we an justly say that leptoni WIMPs have no plae in Partile Physis. 3. Dark Matter does not Exist in Spiral Gala xies As it has been shown by de Souza [15] the onstany of the tangential veloity in spiral arms of spiral galaxies an be explained by the outward expulsion of matter from their enters. And this onstany generates their splendid spiral struture whih an be a logarithmi spiral within ertain onditions. 4. Dark Matter does not Exist in the Milky Way s Neighborhood Kroupa et al. [16] show that the shape of the observed distribution of the Milky Way (MW) satellites is inonsistent with their being drawn from a osmologial substruture population with a onfidene level of 99.5 per ent. Most of the MW satellites therefore annot be related to darkmatter dominated satellites. At the IDM016, the LUX Collaboration reported null results for WIMPs [18]. It is important to emphasize that LUX sensitivity was pushed to a point whih is four times better than that originally projeted. This is a result for WIMPs masses of 50 GeV/. The null results in the low mass region up to 014 have been analyzed by Cerdeño [19] and Cline [0]. 7. The Existing Baryoni Mass in Galaxies is suffiient for Closing the Universe The Universe is full of voids whih are regions with muh less galaxies than the regions surrounding the voids whih are galaxy sheets and walls strething up to many tens of megaparses. Over time as voids expand, matter gets squeezed in between them, and sheets, walls and filaments build the void boundaries [1]. El-Ad et al. [] have reported an average diameter of about 57 Mp (for h=0.7) for voids and Giovanelli [3] has reported that voids have an average density of only 1/10 of the overall average density. The mean density in walls and sheets is at least kg/m 3 [4] whih is muh smaller than the so-alled ritial density given by

3 Journal Heading Year; Vol. (No.): page range 3 3H 8 G (1) Gm4R t Ep Gm4R t (3) R whih is equal to 10-6 kg/m 3 and is alulated onsidering that is valid everywhere inside a homogeneous sphere of radius r and that Hubble s (H) onstant has the same value everywhere inside the sphere, but Hubble s onstant has different values for galaxies inside voids and is different from its value for galaxies in walls and sheets due to the peuliar veloities of galaxies. Therefore, makes no sense beause the expansion is not homogeneous on the sale of a void, and it is exatly the expansions of voids that onur to the whole expansion of the Universe. Suh a alulation with a homogeneous and isotropi spherially symmetrial and with a onstant value for H only makes sense in the beginning of the Universe, and in this ase, the density was muh larger than its value in the loal Universe. Sine galaxies are attrated more and more to the sheets and walls, there is a steep inrease in the density in the walls and sheets. In the alulation below we take into aount the fat that is muh larger in the void boundaries and onsider a ertain void of radius R surrounded by a wall of thikness t whih is muh smaller than R. Thus the total mass of the wall is about MW 4R t () where is the density of matter in the wall ( kg/m 3 ). Therefore, the potential energy of a galaxy of mass m in the wall is and thus the total energy of a galaxy in the wall is 1 (4) E mv Gm4R t in whih v is the peuliar veloity of the galaxy in the wall. We have used Newtonian Mehanis beause, of ourse, the gravitational field in the wall is weak. In order to have a losed Universe, E should be slightly less than zero, so that the limiting veloity, V, is in whih 1/ V GR t (5) 8 M R M the maximum radius that the void an attain in the future whih is an unknown quantity, but we an alulate a lower bound for V by making RM 57 Mp. We take t 7.1 Mp [5] and obtain V= 313 km/s whih is of the order of the peuliar veloities of galaxies in the loal Universe. Tully et al. have reported that galaxies bounding the Loal Void have peuliar veloities +300 km/s [6]. Let us have in mind that may be muh larger beause galaxies may have large amounts of gases around them. Gupta et al. [7] have reently found a huge reservoir of hot gas around the Milky Way, a gas halo, extending to over a distane of 100 kp. The loud ontains large amounts of hydrogen and oxygen. It is not known yet how far the loud goes to and it may extend farther into the surrounding loal group. This gas is probably leftover gas from the original gas loud from whih the Milky Way was born. Of ourse, all galaxies should also have gases around them. An indiation of this is the hot gas seen in lusters [8].

4 4 author name (et al.): artile title There may also be many dwarf galaxies that have not yet been seen. In a very reent artile from last November, Homma et al. [9] report the disovery of a faint satellite of the Milky Way. Therefore, V may be larger than 313 km/s, but still of the same order of magnitude. For example, if the density is doubled, than V 450 km/s. These numbers above may be indiating that the voids may be reahing their largest sizes. Whenever they reah their maximum sizes, they will also get destroyed, and galaxies will rush towards lusters and superlusters. It is important to emphasize that other peuliar veloities have the same order of magnitude of the alulated peuliar veloity above. For example, The Milky Way is falling towards the Virgo luster with a veloity of about 300 km/s and the Loal Superluster is falling towards the Hydra- Centaurus Superluster with a veloity of about 500 km/s (8). 8. Conlusion As shown above dark matter does not exist in the Universe and there is no need for it anyway, for losing the Universe. Besides the gases surrounding galaxies there may also be many dwarf galaxies whih have not yet been aounted for. It is learly shown that the peuliar veloities of galaxies in the loal Universe have the same order of magnitude of the peuliar veloities of galaxies in the walls for losing the Universe. Referenes 1) K. J. Cornelius, "First attempt at a theory of the arrangement and motion of the sidereal system". Astrophysial Journal, vol. 55, 30, 19. ) J. H. Oort, "The fore exerted by the stellar system in the diretion perpendiular to the galati plane and some related problems," Bulletin of the Astronomial Institutes of the Netherlands, vol. 6, 49, ) F. Zwiky, "Die Rotvershiebung von extragalaktishen Nebeln". Helvetia Physia Ata, vol. 6, , ) V. C. Rubin and W. K. Ford, Jr., "Rotation of the Andromeda Nebula from a Spetrosopi Survey of Emission Regions", Astrophysial Journal, vol. 150, 379, ) R. Massey R, J. Rhodes, R. Ellis, N. Soville, A. Leauthaud, A. Finoguenov, P. Capak, D. Baon, H. Aussel, J. P. Kneib, A. Koekemoer, H. MCraken, B. Mobasher, S. Pires, A. Refregier, S. Sasaki, J. L. Stark, Y. Taniguhi, A. Taylor, and J. R. Taylor. "Dark matter maps reveal osmi saffolding", Nature, vol. 445(715), 86, ) J. R. Primak, Dark Matter and Galaxy Formation, AIP Conf. Pro.119, 101, ) LambdaCDM Theory, story/ dmdensity.fm 8) L. D. Duffy and K. van Bibber, Axions as Dark Matter Partiles, New J. Phys. vol. 11,105008, ) R. D. Peei and H. R. Quinn, "CP Conservation in the Presene of Pseudopartiles". Phys. Rev. Lett., vol. 38 (5), 1440, ) R. D. Peei and H. R. Quinn, "Constraints imposed by CP onservation in the presene of pseudopartiles", Phys. Rev. D, vol. 16 (6), 1791, ) J. E. Kim, (1979). "Weak-Interation Singlet and Strong CP Invariane". Phys. Rev. Lett., vol. 43 (): 103, ) M. Shifman, A. Vainshtein, and V. Zakharov, (1980). "Can onfinement ensure natural CP invariane of strong interations?", Nul. Phys. B, vol. 166, 493, ) M. Dine, W. Fishler, and M. Sredniki, "A simple solution to the strong CP problem with a harmless axion", Phys. Lett. B, vol. 104, 199, ) A. Zhitnitsky, "On possible suppression of the axion-hadron interations", Sov. J. Nul. Phys., vol. 31, 60, 1980.

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