ALBERT

Notes: Abstract A formula to compute the mass-height relation for the case of possible antimatter meteor entrance is derived.It is governed by the annihilation cross section for the atom-antiatom interactions which experimentally is unknown,and by various mechanisms which are possibly reducing its value. For the special case of thermal energies,the annihilation cross-section Σan may be connected with the elastic cross-sectionΣel by the relation % MathType!MTEF!2!1!+-% feaafeart1ev1aaatCvAUfeBSjuyZL2yd9gzLbvyNv2CaerbuLwBLn% hiov2DGi1BTfMBaeXatLxBI9gBaerbd9wDYLwzYbItLDharqqtubsr% 4rNCHbGeaGqiVu0Je9sqqrpepC0xbbL8F4rqqrFfpeea0xe9Lq-Jc9% vqaqpepm0xbba9pwe9Q8fs0-yqaqpepae9pg0FirpepeKkFr0xfr-x% fr-xb9adbaqaaeGaciGaaiaabeqaamaabaabaaGcbaGaeq4Wdm3aaS% baaSqaaiaabggacaqGUbaabeaakiabg2da9iabeo8aZnaaBaaaleaa% caqGLbGaaeiBaaqabaGccqGHpis1caWGMbWaaSbaaSqaaiaadMgaae% qaaaaa!4227!\[\sigma _{{\rm{an}}} = \sigma _{{\rm{el}}} \prod f_i \],where the factors % MathType!MTEF!2!1!+-% feaafeart1ev1aaatCvAUfeBSjuyZL2yd9gzLbvyNv2CaerbuLwBLn% hiov2DGi1BTfMBaeXatLxBI9gBaerbd9wDYLwzYbItLDharqqtubsr% 4rNCHbGeaGqiVu0Je9sqqrpepC0xbbL8F4rqqrFfpeea0xe9Lq-Jc9% vqaqpepm0xbba9pwe9Q8fs0-yqaqpepae9pg0FirpepeKkFr0xfr-x% fr-xb9adbaqaaeGaciGaaiaabeqaamaabaabaaGcbaGaamOzamaaBa% aaleaacaWGPbaabeaaaaa!37F1!\[f_i \]are all less or equal to unity. Among them, the most significant is the barrier factor % MathType!MTEF!2!1!+-% feaafeart1ev1aaatCvAUfeBSjuyZL2yd9gzLbvyNv2CaerbuLwBLn% hiov2DGi1BTfMBaeXatLxBI9gBaerbd9wDYLwzYbItLDharqqtubsr% 4rNCHbGeaGqiVu0Je9sqqrpepC0xbbL8F4rqqrFfpeea0xe9Lq-Jc9% vqaqpepm0xbba9pwe9Q8fs0-yqaqpepae9pg0FirpepeKkFr0xfr-x% fr-xb9adbaqaaeGaciGaaiaabeqaamaabaabaaGcbaGaamOzamaaBa% aaleaacaWGIbaabeaaaaa!37EA!\[f_b \] b described by many scientists, which may possibly reduce the annihilation cross-section down to lower than 10−11 times than that of a simple elastic collision. The above formula could also be found useful, for some applications, which are currently in progress.

Notes: Abstract The momentum loss for a possible antimatter meteor entrance can be described by the combination of two terms. One which can be characterized by the mechanism of annihilation and a second one, the well known mechanism, which is common for all koinomatter (ordinary) meteors. That is, the momentum loss caused by the air molecules swept up by the moving object. We discuss, in this paper, the contribution of the rocket effect caused by the action of the secondaries which can be produced by the annihilation interactions of the antiatoms with the air molecules. The momentum loss of an iron type meteor made of antimatter, as a function of its equivalent radius R, can be described by the formula, δJ (MeV/c) = 8R (cm), for values of R within the range 1 cm 〈 R 〈 5 cm and can be resulted by a single annihilation interaction of a nucleon-antinucleon pair.

Notes: Abstract Antimatter meteors, like ordinary ones, can be heated during their infall flight. However, this could happen by a completely different process than in the case of koinomatter meteors, since in the latter case the annihilation interactions mechanism is absent. In case of antimatter meteors, the temperature may be increased mainly due to the energy deposition effect, caused by the passage of the annihilation secondaries penetrating throughout the meteor. The energy deposition of the secondary particles produced in matter antimatter annihilation interactions as a function of the dimensions of an antimatter meteor is described in this paper.

Notes: Abstract The lifetime of antimatter fragments which may enter the Earth's atmosphere in the form of meteors is determined in this paper, for cases in which the annihilation may be accompanied by the evaporation process. The antimatter object can be penetrated by the nucleon - antinucleon annihilation products, which can be generated by interactions of atoms of antimatter fragments with the atmospheric molecules. Vaporization of its own antiatoms may be followed, in case of a high rate of annihilation, so that the lifetime of the antimatter object may become shorter, compared with the case of annihilation without vapor production of the meteor. The lifetime of the antimatter fragment is dependent upon the temperature of the object and thus vaporization of such an object would last for as long asδτ =Rδ/ξ, whereξ is the intensity of evaporation,δ its density andR its radius.

Notes: Abstract Antimatter meteors probably enter the Earth's atmosphere. If they have the ability to escape complete vaporization during their infall flight, it may be possible, that a fraction of their original mass could survive for short or long time, depending on the mechanisms of ablation. In case of ablation through the annihilation process only, the lifetimeδτ of such an object is following the simple relationδτ = (N L Rδ)/(rA), whereδ andA are the density and the atomic weight of the antimatter fragment respectively,R is its radius,r is the rate of annihilation per cm2 of its surface, and N L is the Loschmidt number.

Notes: Abstract A comparison of multiplicity distributions and $$\left\langle {P_T^2 } \right\rangle of \bar pp$$ annihilation reactions at two energies ande + e −→hadrons leads to a model for $$\bar pp$$ annihilation into gluons. The $$\bar pp$$ data are consistent with the QCD predictions for the ratio of the moments of the fragmentation functions given for isolated gluon jets. The energy dependence of the ratio of the moments is also consistent with the predictions.

Notes: Abstract A general velocity-height relation for both antimatter and ordinary matter meteor is derived. This relation can be expressed as % MathType!MTEF!2!1!+-% feaafiart1ev1aaatCvAUfeBSjuyZL2yd9gzLbvyNv2CaerbuLwBLn% hiov2DGi1BTfMBaeXatLxBI9gBaerbd9wDYLwzYbItLDharqqtubsr% 4rNCHbGeaGqiVu0Je9sqqrpepC0xbbL8F4rqqrFfpeea0xe9Lq-Jc9% vqaqpepm0xbba9pwe9Q8fs0-yqaqpepae9pg0FirpepeKkFr0xfr-x% fr-xb9adbaqaaeGaciGaaiaabeqaamaabaabaaGcbaWaaSaaaeaacq% aHfpqDdaWgaaWcbaGaamOEaaqabaaakeaacqaHfpqDdaWgaaWcbaGa% eyOhIukabeaaaaGccqGH9aqpcaqGLbGaaeiEaiaabchacaqGGaWaam% WaaeaacqGHsisldaWcaaqaaiaadkeaaeaacaWGHbaaaiaabwgacaqG% 4bGaaeiCaiaabIcacaqGTaGaamyyaiaadQhacaGGPaaacaGLBbGaay% zxaaGaeyOeI0YaaSaaaeaacaWGdbaabaGaamOqaiabew8a1naaBaaa% leaacqGHEisPaeqaaaaakmaacmaabaGaaGymaiabgkHiTiaabwgaca% qG4bGaaeiCamaadmaabaGaeyOeI0YaaSaaaeaacaWGcbaabaGaamyy% aaaacaqGLbGaaeiEaiaabchacaqGOaGaaeylaiaadggacaWG6bGaai% ykaaGaay5waiaaw2faaaGaay5Eaiaaw2haaiaacYcaaaa!64FD!\[\frac{{\upsilon _z }}{{\upsilon _\infty }} = {\text{exp }}\left[ { - \frac{B}{a}{\text{exp( - }}az)} \right] - \frac{C}{{B\upsilon _\infty }}\left\{ {1 - {\text{exp}}\left[ { - \frac{B}{a}{\text{exp( - }}az)} \right]} \right\},\]where υ z is the velocity of the meteoroid at height z, υ∞ its velocity before entrance into the Earth's atmosphere, α is the scale-height, and C parameter proportional to the atom-antiatom annihilation cross- section, which is experimentally unknown. The parameter B (B = DAϱ0/m) is the well known parameter for koinomatter (ordinary matter) meteors, D is the drag factor, ϱ0 is the air density at sea level, A is the cross sectional area of the meteoroid and m its mass. When the annihilation cross-section is zero — in the case of ordinary meteors — the parameter C is also zero and the above derived equation becomes % MathType!MTEF!2!1!+-% feaafiart1ev1aaatCvAUfeBSjuyZL2yd9gzLbvyNv2CaerbuLwBLn% hiov2DGi1BTfMBaeXatLxBI9gBaerbd9wDYLwzYbItLDharqqtubsr% 4rNCHbGeaGqiVu0Je9sqqrpepC0xbbL8F4rqqrFfpeea0xe9Lq-Jc9% vqaqpepm0xbba9pwe9Q8fs0-yqaqpepae9pg0FirpepeKkFr0xfr-x% fr-xb9adbaqaaeGaciGaaiaabeqaamaabaabaaGcbaWaaSaaaeaacq% aHfpqDdaWgaaWcbaGaamOEaaqabaaakeaacqaHfpqDdaWgaaWcbaGa% eyOhIukabeaaaaGccqGH9aqpcaqGLbGaaeiEaiaabchacaqGGaWaam% WaaeaacqGHsisldaWcaaqaaiaadkeaaeaacaWGHbaaaiaabwgacaqG% 4bGaaeiCaiaabIcacaqGTaGaamyyaiaadQhacaGGPaaacaGLBbGaay% zxaaGaaiilaaaa!4CF5!\[\frac{{\upsilon _z }}{{\upsilon _\infty }} = {\text{exp }}\left[ { - \frac{B}{a}{\text{exp( - }}az)} \right],\]which is the well known velocity-height relation for koinomatter meteors. In the case in which the Universe contains antimatter in compact solid structure, the velocity-height relation can be found useful.