Condensate of excitations in moving superfluids

A possibility of the condensation of excitations with a non-zero momentum in rectilinearly moving and rotating superfluid bosonic and fermionic (with Cooper pairing) media is considered in terms of a phenomenological order-parameter functional at zero and non-zero temperature. The results might be applicable to the description of bosonic systems like superfluid $^4$He, ultracold atomic Bose gases, charged pion and kaon condensates in rotating neutron stars, and various superconducting fermionic systems with pairing, like proton and color-superconducting components in compact stars, metallic superconductors, and neutral fermionic systems with pairing, like the neutron component in compact stars and ultracold atomic Fermi gases. Order parameters of the"mother"condensate in the superfluid and the new condensate of excitations, corresponding energy gains, critical temperatures and critical velocities are found.

condensate of zero-sound-like excitations with non-zero momentum in the description of the stability of r modes in rapidly rotating pulsars was discussed in [7].
The key idea of the phenomenon is the following [1,2]: When a medium moves as a whole with respect to a laboratory frame with a velocity higher than v L c , it may become energetically favorable to transfer a part of its momentum from particles of the moving medium to a Bose condensate of excitations (CoE) with a non-zero momentum k = 0. It would happen, if the spectrum of excitations is soft in some region of momenta. References [1,6] studied the condensation of excitations at T = 0 assuming the conservation of a flow velocity. Alternatively, we consider systems at other conditions, assuming the conservation of the momentum (or angular momentum for rotating systems) as in [2]. We consider bosonic and fermionic superfluid systems moving initially with the flow velocity above v L c both for T = 0 and T = 0 (the latter case was not yet considered in mentioned references), taking into account a back reaction of the CoE on the "mother" condensate of the superfluid.
The work is organized as follows. In Sect. 2 we construct the phenomenological orderparameter functional for the description of the CoE coupled with the mother condensate in the superfluid moving linearly with the flow velocity exceeding v L c . Section 3 is devoted to the description of cold moving superfluids. Section 4 studies peculiarities of the two-fluid motion in warm superfluids in the presence of the CoE. In Sect. 5 we discuss a particular role of vortices. Some numerical estimations valid for fermion superfluids in the BCS limit and for He-II are performed in Sect. 6. Section 7 describes the CoE in rotating systems with application to the rapidly rotating pulsars. Section 8 contains concluding remarks.

Order-parameter functional for moving fluid
In the spirit of the Landau phenomenological theory of a second-order phase transition the free-energy density of the superfluid subsystem in its rest frame can be expanded in the order parameter ψ for temperatures T ≤ T c , where T c is the critical temperature of the second-order phase transition, [9,10]: Here a T ≥ 0, b T > 0 and c T > 0 are phenomenological parameters depending on the temperature, so that a T vanishes at T = T c . When applied to superconductors the functional (1) is known in the literature as the Ginzburg-Landau model [9], while for the case of the superfluid 4 He it is called the Ginzburg-Pitaevskii model. The phenomenological description of cold weakly interacting Bose gases was performed by Gross and Pitaevskii, see [9]. As pointed out in ref. [10], the expansion in the order parameter is a primary feature in the 2/15 Landau's phase-transition theory, whereas an expansion in powers of (T c − T ) is a secondary assumption. Therefore, we will use the functional (1) for all T < T c . For 0 < t = 1 − T /T c ≪ 1, the coefficients a T and b T can be expanded as [10] a T = a 0 t α , b T = b 0 t β , and c T is usually assumed to be constant, c T = c 0 . Within the mean-field approximation from the Taylor expansion of F L in t ≪ 1 it follows that α = 1, β = 0. The width of the fluctuation region, wherein the mean-field approximation is not applicable, is evaluated with the help of the Ginzburg [10] and Ginzburg-Levanyuk [22] criteria. For the ordinary metallic superconductors the fluctuation region proves to be usually very narrow and the mean-field approximation holds then for almost any temperatures below T c , except a tiny vicinity of T c . Thus, for t ≪ 1, neglecting the mentioned narrow fluctuation region, one may use α = 1, β = 0. For He-II, fluctuations prove to be important for all temperatures below T c , cf. [10]. Using the experimental fact that the specific heat of the He-II has no power divergence at T → T c , we get α = 4/3 and β = 2/3 that coincides with phenomenological findings [10].
Consider a system at a finite temperature consisting of normal and superfluid parts undergoing rectilinear motions parallel to a wall. The wall singles out the laboratory frame with respect to which the motion is defined. Interactions between particles in normal fluid may lead to creation of excitations. Mechanisms of the excitation production depend on the specifics of problems and will be discussed below in Sects. 4, 5, and 7.
We assume that the superfluid moves with an initial velocity v with respect to the wall and additionally the excitations can carry some net momentum, j n , with respect to the superfluid. Then one can define an average velocity of the excitations with respect to the superfluid component w. With respect to the wall the excitations have the average velocity v n = w + v. The motion of the superfluid as a whole with velocity v relative to the reference frame of the wall can be described by introducing the phase of the condensate field ψ = |ψ|e iφ with v = ∇φ/m .
We can write the variational functional for the condensate field in the standard form of the two-fluid model [11] The density of the superfluid component, which determines the amplitude of the condensate field ψ is related to the normal component ρ n by the relation where m is the mass of the pair for systems with pairing, and the mass of a boson in bosonic superfluids, e.g., the mass of the 4 He atom in case of the He-II. The quantity F bind in Eq. (2) stands for a binding free-energy density of the normal subsystem in its rest frame, which explicit form is not of our interest here. The first term in (2) can be hidden in F L [ψ] as a phase of the condensate field. For the case when the normal component rests, v n = 0, i.e., the superfluid moves with the velocity v = − w, the minimization of the functional (2) gives and, hence, the critical temperature decreases with a velocity increase as T c (w) = T c (1 − mw 2 /(2a 0 )) [23] and vanishes at w = w A = (2a 0 /m) 1/2 . In reality the superfluid flow j s = vρ s = vρ − j n becomes unstable with w = 0 even at the smaller velocity w A1 , determined 3/15 from the condition ∂j s (T, w)/∂w = 0, see [24,25]. In general w A is smaller than v L c [24] and for small t one finds [10,24] w A1 ≈ (2 a T / (3m)) 1/2 ≪ v L c . Thus, for a flow in a narrow pipe, in the equilibrium state with v n = 0 and hence w = v, the CoE would not appear since the mother condensate is destroyed already for v = w A1 < v L c . Therefore, in further discussion we assume that w < w A1 . Situations, in which the latter condition is fulfilled, will be discussed later in the text. In case w < w A1 of our interest the finite value of w implies only a redefinition of the critical temperature T c → T c (w). Thereby, to simplify further notations we put w = 0. The generalization is straightforward. Then the free-energy density functional of the system moving with the velocity v respectively the wall is given by The equilibrium volume-averaged value of the condensate is given then by Eq. (4) and the volume-averaged density of the normal component,ρ n , is related to the averaged total density of the fluid,ρ, asρ n =ρ − m |ψ eq | 2 . The equilibrium value of the volume-averaged free-energy density (we shall call it as an "in"-state) is When the speed of the flow v exceeds the Landau critical velocity, on top of the mother condensate ψ there may appear in the fluid a CoE ψ ′ [1, 2, 6] with the frequency ǫ(k 0 ) and momentum k 0 calculated in the rest frame of the superfluid, where, as we have assumed, the ratio ǫ(k)/k has minimum at k = k 0 = 0. For He-II the spectrum ǫ(k) is the standard phonon-roton spectrum, normalized as ǫ(k) ∝ k for small k. In the case of the straightforward motion, we, following the symmetry arguments, may choose the simplest form of the CoE order parameter depending on the time τ and the coordinate r as with a constant amplitude ψ ′ 0 for the homogeneous system that we consider. For the description of CoE with the given frequency ǫ(k 0 ) the functional (1) must be supplemented by the functional F ex [ψ] involving higher gradient terms so that the variation of the Fourier transform of the full functional reproduces the excitation frequency and the self-interaction parameters of the CoE free-energy density functional: For example, in ref. [6] these parameters were estimated for a cold weakly interacting Bose gases. The explicit structure of F ex is not important for our study as we use the phenomenological parameters b ′ T,k0 , and b ′′ T,k0 .

4/15
We suppose that, when the CoE is formed (we shall call it a "fin"-state), the initial momentum density is redistributed between the fluid and the CoE: Here k 0 |ψ ′ 0 | 2 is the momentum density carried by the CoE in the rest frame of the superfluid, ( k 0 + m v fin )|ψ ′ 0 | 2 is the resulting momentum density carried by the CoE in the laboratory frame and the first term, (ρ − m |ψ ′ 0 | 2 ) v fin , is the resulting momentum density carried by the superfluid in the laboratory frame. So, the CoE necessarily moves in the laboratory frame.
In the presence of the CoE the resulting order parameter ψ fin is the sum of the mother condensate, ψ, and of the CoE, ψ ′ , ψ fin = ψ + ψ ′ . The volume-averaged free-energy density of the system with the CoE,F fin =F L [ψ fin ] +F ex [ψ fin ], can be written as whereǫ(k) is the energy of the excitation including the mean-field potential, . Now, using the momentum conservation (8) we express v fin through v and get for the change of the averaged free-energy density associated with the CoE, where we put k 0 v . We apply now the functional (10) to superfluids for T → 0 and T = 0.

bosonic system
At T → 0 the whole medium is superfluid and amplitudes of the condensates are constrained by the spatially averaged particle number densitȳ In the presence of the CoE the density becomes spatially oscillating around its averaged value. For a weak condensate, i.e., |v − v L c | ≪ v L c , we find perturbatively The density modulation was predicted in [1] and reproduced in the numerical simulation of the supercritical flow in He-II using a realistic density functional [5]. Replacing Eq. (11) in (10) and putting T = 0 we find the change of the spatially-averaged energy density of the system because of the appearance of the CoE, δĒ =Ē fin −Ē in , where are considered above coefficients taken now for T = 0. Minimizing this functional with respect to ψ ′ 0 we obtain 5 /15 From (8) we find that because of the CoE with k = 0 the flow is decelerated to the velocity The volume-averaged energy gain due to appearance of the CoE is If χ 0 > 0, one has v fin < v L c . As we estimate below in case of He-II and in case of the BCS weak coupling, the parameter |χ 0 | ≪ 1 and v fin ≃ v L c . As follows from Eq. (16) the CoE appears in a second-order phase transition since dδĒ The amplitude of the CoE (14) grows with the velocity, whereas the amplitude of the mother condensate decreases. The value |ψ| 2 vanishes when v = v c2 , the second critical velocity, at which |ψ ′ 0 | 2 =n according to Eq. (11). The value v c2 is evaluated from (14) as When the mother condensate disappears at v = v c2 , the excitation spectrum is cardinally reconstructed, and the superfluidity destruction occurs as a first-order phase transition. We assume that for v > v c2 the excitation spectrum has no low-lying local minimum at a finite momentum. Then the amplitude |ψ ′ 0 | 2 jumps fromn to 0 and δĒ jumps from

fermionic system
As shown in refs. [17,18,26], in fermionic systems with pairing there may exist bosonic modes with suitable spectra, supporting quasiparticle excitations with the energy ≃ 2∆ and momentum k 0 ≃ 2p F , ∆ is the pairing gap computed in the rest frame of the superfluid, see Fig. 2 in [17], and Fig. 4 in [18]. For these modes the Landau critical velocity is and for v > v L c there is a chance for the condensation of the bosonic excitations as we considered above.
Besides bosonic excitations there exist fermionic ones with the spectrum ǫ f (p) = Stemming from the breakup of Cooper pairs, the fermionic excitations are produced pairwise and the corresponding (fermion) Landau critical velocity is . The latter expression reduces to [27] v We see that up to a small correction of the order of ( For T → 0 the fermionic excitations are produced near the wall and move, therefore, with respect to the superfluid with the velocity − v. 1 Hence, the change of the energy density due to the Cooper pair breaking can be calculated as Expanding this integral for velocities v close to the critical velocity v L c ≈ v L c,f we find being valid for v ≪ v F . Since the critical velocity v L c,f is slightly smaller than v L c , Eq. (20) wins over Eq. (16) for ] the formation of the CoE becomes energetically more favorable than the pair breaking. Although the above estimates are applicable only for 0 < v/v L c − 1 ≪ 1, there is another argument in favour of the condensation of bosonic excitations. In a system, in which the normal component (fermionic excitations) moves relative to superfluid with the velocity w the pairing gap decreases (Rogers-Bardeen effect [28]). In the case under consideration a superfluid moves with the velocity v > v L c relative to the wall. Excitations are produced near the wall, and the pairing gap decreases, being determined by the equation [29] ln For With the subsequent growth of v (for v/v L c − 1 > ∼ 1) the gap continues to decrease and, as follows from Eq. (21), it vanishes at v = v L c2,f = e 2 v L c , see [29]. Since in the presence of the CoE the final velocity of the flow is v fin = v L c and the gap does not change, the additional gain in the energy density due to the formation of the condensate of bosonic excitations compared to the pair breaking without the CoE formation is where [9] F eq L (T = 0, ∆) = − m * pF 4π 2 ∆ 2 . For 0 ≤ v/v L c − 1 ≪ 1 by substituting Eq. (22) in Eq. (23) and rewriting m * pF For v > v L c2,f one has ∆(v) = 0, and, as follows from Eq. (23), the gain in the energy density because of the CoE compared to the full destruction of the pairing would be δĒ gap = −3ρ(v L c ) 2 /4. Thus we can conclude that the creation of the condensate of bosonic excitations with finite momentum in moving cold fermionic systems with pairing leading to a reduction of the flow velocity is energetically more profitable than the breaking of Cooper pairs and the decrease of the pairing gap.

Warm superfluid. Two-fluid motion
Only for a very low T the normal component can be neglected. For a higher temperature the normal subsystem serves as a reservoir of particles for the formation of the mother and daughter condensates, which amplitudes are now to be chosen by minimization of the free 7/15 energy of the system. Therefore, minimizing (10), we vary now ψ and ψ ′ 0 independently and find The quantity T c stands for the renormalized critical temperature, which depends now on the flow velocity, and v c2 (T ) stands for the second critical velocity depending on T . The condition |ψ| 2 = 0 implies the relation between v and The solution of this equation for the velocity, v c2 (T ), increases with the decreasing temperature, and the solution for the temperature, T c (v), decreases with increasing v. At T = T c (v) or v = v c2 (T ) we have |ψ| 2 = 0 but |ψ ′ 0 | 2 = 0, and for T > T c (v) or for v > v c2 (T ) the condensate |ψ ′ 0 | 2 vanishes, as for |ψ| 2 = 0 the spectrum of excitations does not contain a suitable lowlying branch. Thus, the superfluidity is destroyed at T = T c (v) or v = v c2 (T ) in a first-order phase transition.
From Eqs. (8) and (25) we find for v > v L c and χ T < 1 the resulting velocity of the flow similar to Eq. (15) obtained above for T = 0. If χ T > 0, one has v fin < v L c , and v fin ≃ v L c for 0 < χ T ≪ 1.
Substituting the order parameters from (25) in (10), we find for the averaged free-energy density gain owing to the appearance of the CoE for χ T < 1 . Thus, for v L c < v < v c2 the free energy decreases owing to the appearance of the CoE with k = 0 in the presence of the non-vanishing mother condensate. The value of k 0 is to be found from the minimization of Eq. (28). As T c , the momentum k 0 gets renormalized and differs now from the value corresponding to the minimum of ǫ(k)/k. As for T = 0, for T = 0 the CoE appears at v = v L c in a second-order phase transition but it disappears at v = v c2 in a first-order phase transition with jumps from to 0.
At finite temperature the dynamics of the CoE amplitude can be determined from the equation [30] where Γ is a formation rate of the CoE. In the theory of non-equilibrium superconductors this equation is known as the time-dependent Ginzburg-Landau equation. Note that the 8/15 dynamics following this equation is different from that follows from the Gross-Pitaevskii equation describing a weakly non-ideal Bose gas in an external field. It is determined by the time-dependence of the potential. We emphasize that the above consideration assumes that the formation rate Γ of the CoE is faster than the deceleration rate 1/τ norm fr of the normal subsystem. The former time 1/Γ is of a microscopic origin, whereas τ norm fr might be very large as being caused by the friction force between the normal component and the wall. For rotating compact stars τ norm fr is determined by the decay of a star magnetic field yielding τ norm fr > ∼ 10 3 yrs [16] for magnetic fields below 10 13 G. Thus, the COE has enough time to be developed in mentioned cases.
When the fluid flowing with v > v L c at T > T c (v) is cooled down to T < T c (v), it consists four components: the normal excitations, the superfluid, the vortices and the CoE, all moving rigidly with v fin < v L c (if χ T > 0). If the system is then rapidly re-heated to T > T c (v), the superfluid component, the vortices and the CoE vanish and the remaining normal fluid consists of two fractions: one still moving with v fin ( T c ) < v L c , owing to conservation of the momentum, and the other one, being originated from the melted CoE, with the mass equal to ma( T c )/(2b ′ T,k0 ( T c )), moving with a higher velocity until a new equilibrium is established. This may show one of possibilities how one could identify formation of the CoE experimentally.
Note that for fermion superfluids at T = 0 after the CoE is formed the flow velocity (the estimate is done for χ T = 3b 0ρ /k 2 0 ), and hence the Cooper pair breaking does not occur, whereas the condensate of Bose excitations is preserved.

Vortices
Above we focused our consideration on the cases where either the vortices are absent (as in a narrow capillary [1]) or they leave the system (in open systems), or the presence of vortices supports a common rigid motion of the normal and superfluid components [20] (e.g., as in systems with charged components [31], or in rotating systems, like neutron stars [16]).
In case of He-II moving in a narrow capillary vortices do not appear, see [1,5]. For a rectilinearly moving superfluids in extended geometry there may appear excitations of the type of vortex rings and other structures [32]. The energy of the ring is estimated [10,11] as ǫ vort = 2π 2 2 |ψ| 2 R m −1 ln(R/ξ), and the momentum is p vort = 2π 2 |ψ| 2 R 2 , where R is the radius of the vortex ring and ξ is the coherence length, ξ ∼ (c T /a T ) 1/2 , as estimated above. Thus, v c1 = ǫ vort /p vort = (R t m) −1 ln(R t /ξ) is the Landau critical velocity for the vortex production, where in the absence of impurities R t is of the order of the transverse size of the system. For a system of distributed impurities moving together with the fluid, R t is a typical distance between the defects. Vortices are pined to the impurities and move together with them and the superfluid. In an open clean system at v > v c1 the vortex rings are pushed to infinity by Magnus and Iordanskii forces. Note that for spatially extended systems the value v c1 is lower than the Landau critical velocity v L c . The flow moving with the velocity v for v c1 ≤ v may be considered as metastable, since the vortex creation probability is hindered by a large potential barrier and formation of a vortex takes a long time [33]. The vortex production rate increases, however, strongly when v approaches v L c [33]. For a motion in a pipe the vortices are captured by the pipe wall, forming after a while a stationary subsystem in the frame of the walls. Periodic solitonic solutions of the Gross-Pitaevskii equation were studied in [34]. This situation might be rather similar to that of a mother condensate moving 9/15 in a periodic potential, produced by the spatial variations of the CoE order parameter [6]. Since in exterior regions of the vortices the superfluidity persists, our consideration of the condensation of excitations for v L c < v is applicable. Note that in He-II under a high external pressure v L c decreases and at some conditions becomes lower than v c1 , see [35], and in the interval v L c < v < v c1 there are no vortices but the CoE may appear. In superconducting systems vortices if formed, are involved in a common motion with the superconducting subsystem due to the appearance of a tiny London field [31] distributed throughout the medium, that supports the condition w = 0.
In rotating superfluids vortices appear at rotation frequency Ω > Ω c1 = m R 2 ln(R/ξ), where for the spherical system R is the size of the system (transversal size for the cylindrical system), and their number grows with an increase of Ω. When the density of vortices becomes sufficiently large, they form a lattice, cf. [20], forcing, thereby, the superfluid and normal components to move as a rigid body, i.e. with w → 0.

Estimates for fermionic and bosonic superfluids
We apply now the expressions derived in the previous sections to several practical cases.

fermionic syperfluid
Consider a fermion system with the singlet pairing. In the weak-coupling (BCS) approximation the parameters of the functional (1) can be extracted from the microscopic theory [9]: where m * F stands for the effective fermion mass (m * F ≃ m F in the weak-coupling limit), n = p 3 F /(3π 2 3 ) is the particle number density, and the fermion chemical potential is µ ≃ ǫ F = p 2 F /(2m * F ). The function ζ(x) is the Riemann ζ-function and ζ(3) = 1.202. With the BCS parameters we have |ψ| 2 = nt and the pairing gap ∆ = T c 8π 2 t 7ζ(3) , see [21]. With parameters (31) we estimate b 0ρ /k 2 0 = 3∆ 2 /(8v 2 F p 2 F ) and a 0 /k 0 = 3∆ 2 /(4v F p 2 F ) , whereρ ≃nm F . We see that if b ′ T,k0 ∼ b ′′ T,k0 ∼ b T one gets 0 < χ T = 3b Tρ /k 2 0 ≪ 1, since the latter inequality is reduced to the inequality ∆ ≪ ǫ F , which is well satisfied. In this limit |ψ ′ 0 | 2 given by Eq. (25) gets the same form as Eq. (14). The resulting flow velocity after condensation of excitations, (27), is lower than v L c but close to it. Since for the BCS case we have α = 1, β = 0, Eq. (26) for the new critical temperature is easily solved, for v > v L c , In the last equality we put b ′ T,k0 = b 0 . We also estimate the maximal second critical velocity

bosonic superfluid on example of He-II
We turn now to the bosonic superfluid, He-II. In He-II there exists a branch of the phononroton excitations [9,10]. The typical energy of the rotonic excitations ∆ r = ǫ(k r ) at the roton minimum k = k r depends on the pressure and temperature. According to [36], for 10/15 and c = c 0 = 1/m * ≃ 1/m, with the helium atom mass m = 6.6 · 10 −24 g. The parametrization holds for 10 −6 < t < 0.1, but for rough estimates can be used up to t = 1. For instance, using Eq. (1) we evaluate the He-II mass-density as ma 0 /b 0 ≃ 0.3 g/cm 3 , which is of the order of the experimental value ρ He = 0.15 g/cm 3 at P = 0.
Taking into account that we deal with the rotonic excitation, i.e., k 0 ≃ k r and ǫ(k 0 ) ≃ ∆ r , we estimate, T,k0 ≃ 3.3b T , and assuming b ′ T,k0 ∼ b T we again estimate 0 < χ T ≪ 1. Using the results of [36] wheret = T /T c . Using χ T (He-II) ∼ χ T (BCS), we evaluate condensate amplitudes and the final flow velocity as functions of temperature and depict them in Fig. 1. The CoE appears at v = v L c in a second-order phase transition. For v > v L c the amplitude of the condensate |ψ ′ 0 | 2 (|ψ| 2 ) increases (decreases) linearly with v. The closer T is to T c , the steeper the change of the condensate amplitudes is. The final velocity of the flow, which sets in after the appearance of the CoE, decreases with the increase of v. With α = 4/3, β = 2/3 the renormalized critical temperature determined by Eq. (26) is mother condensate |ψ| 2 vanishes when v reaches the value v c2 , which depends on the temperature as v c2 ≈ v L c (t) + (363t 2/3 − 23.5t 4/3 )m/s. At v = v c2 the superfluidity disappears in a first-order phase transition. The corresponding energy release can be estimated from (29) as δF (v c2 ) ≈ 47a 2 0 8b0 t 4/3 ≃ 5.9 t 4/3 (T c ∆C p ), where ∆C p = 0.76 · 10 7 erg/(cm 3 K) is the specific heat jump at T c [10].

Rotating superfluids. Pulsars
The novel phase with the CoE may also exist in rotating systems. Here, excitations can be generated because of the rotation. Now we should use the angular momentum conservation instead of the momentum conservation. Also, the structure of the order parameter is more complicated than the plane wave. For the cylindrical geometry a probing CoE function can be taken in the form [2] wherer and φ are the polar coordinates and α and β are variational parameters. The value of the critical angular velocity for the appearance of the first vortices, Ω c1 ∼ v c1 /R, proves to be very low for systems of a large size R, e.g. like neutron stars. With these modifications, the results, which we obtained above for the motion with the constant v, continue to hold.
In the inner crust and in a part of the core of a neutron star, protons and neutrons are paired in the 1S 0 state owing to attractive pp and nn interactions, cf. [16]. In denser regions of the star interior the 1S 0 pairing disappears but neutrons might be paired in the 3P 2 state. The charged pp superfluid component should co-rotate with the normal matter. This, as we have mentioned, is due to the appearance of a tiny magnetic field h = 2m p Ω/e p (London effect) in the whole volume of the superfluid, m p (e p ) is the proton mass (charge) [31]. This tiny field, being < ∼ 10 −2 G for the most rapidly rotating pulsars, has no influence on parameters of the star and can be neglected.
With the typical neutron star radius, R ∼ 10 km, and for ∆ ∼MeV typical for the 1S 0 nn pairing, we estimate Ω c1 ∼ 10 −14 Hz. For Ω ≫ Ω c1 the neutron star contains arrays of neutron vortices with regions of the superfluidity in between them, and the star rotates as a rigid body. The vortices would completely overlap, only if Ω reached unrealistically large value Ω vort c2 ∼ 10 20 Hz. The most rapidly rotating pulsar PSR J1748-2446ad has the angular velocity 4500 Hz [37]. The value of the critical angular velocity for the formation of the CoE in the neutron star matter is Ω c ∼ Ω L c ≃ ∆/(p F R) ∼ 10 2 Hz for the pairing gap ∆ ∼ MeV and p F ∼ 300 MeV/c at the nucleon density n ∼ n 0 , where n 0 ≃ 0.17fm −3 is the density of the atomic nucleus, and c is the speed of light. The superfluidity will coexist with the CoE and the array of vortices until the rotation frequency Ω reaches the value Ω c2 > Ω L c , at which both the CoE and the superfluidity disappear completely. From Eq. (26) with the BCS parameters we estimate Ω c2 ∼ v c2 /R < ∼ 10 4 Hz. There are many other millisecond pulsars in low-mass X-ray binaries of a typical age > ∼ 10 8 yrs. Thus, in the detected rapidly rotating pulsars the CoE might coexist with superfluidity, that would also affect their hydrodynamical description [38]. A possible influence of the CoE on the window of the r-mode instability in the millisecond pulsars was recently studied by us in [7]. Also a CoE may appear in the presence of a charged pion condensate with a finite momentum in massive neutron stars [15], see a discussion of an additional 12/15 slowing down of the pulsar which may arise owing to the presence of the π + condensation in [2]. In massive neutron stars there may also exist K − and/orK 0 condensates with a finite momentum, cf. [13,14]. A similar effect to that on a charged pion condensate may exist on K − andK 0 condensates. Another interesting issue is a possibility of the formation of CoEs in color-superconducting regions of rotating hybrid stars. Various CoEs may arise there since pairing gaps between quarks of different colors and flavors may have essentially different values, e.g. in 2SC, 2SC+X, color spin locking, and other possible phases, see in [39].

Conclusion
In this paper we studied a possibility of the condensation of excitations with k = 0, when a superfluid initially flows with respect to a wall with a velocity v larger than the Landau critical velocity v L c . In difference with Refs. [1,5,6], which studied bosonic superfluid systems for T = 0 at a fixed velocity v, we considered this phenomenon for bosonic and fermionic superfluid systems both for T = 0 and T = 0 at the conserving momentum for a rectilinear motion (at the conserving angular momentum for a rotation). In the presence of the CoE the final velocity of the superfluid v fin becomes less than v. Also, compared to Refs. [1,2,5] we incorporated the interaction between the CoE and the "mother" condensate of the superfluid. We studied the case of T ≪ T c , when the normal component can be neglected, and the case of higher T , when it serves as a reservoir of particles affecting the formation of the mother condensate and CoE. The latter case was not enlighten yet in the literature.
At finite temperatures we first studied the systems where the superfluid and normal components move with respect to each other with a relative velocity w (the average velocity of excitations with respect to the superfluid component), and then focused on the case of w = 0. Note that at finite T the mother condensate may exist only for very low values of w (much less than the Landau critical velocity). In rotating superfluids vortices form a lattice and the system rotates as a rigid body. Also, charged subsystems are forced to move as a whole owing to a London force. These are conditions when indeed one can put w = 0.
A back reaction of the CoE on the mother condensate proves to be important both for T = 0 and for T = 0. We found that the CoE appears in a second-order phase transition at v = v L c and the condensate amplitude grows linearly with the increasing velocity. Simultaneously the mother condensate decreases and vanishes at v = v c2 , then the superfluidity is destroyed in a first-order phase transition with an energy release. For v L c < v < v c2 the resulting flow velocity is v fin < v L c . We found that for the cold fermion systems with pairing the creation of the condensate of bosonic excitations with finite momentum, leading to a reduction of the flow velocity up to the value of the Landau critical velocity v L c , is energetically more profitable than the breaking of Cooper pairs appearing for v > v L c,f (v L c > v L c,f ) and the decrease of the pairing gap (except the case when initial velocity v is in a narrow vicinity of the critical point). To the best of our knowledge possibility of condensation of bosonic excitations with finite momentum in moving fermionic systems with pairing was not yet considered in the literature. For fermion superfluids at T = 0 after the CoE is formed the flow velocity becomes less than v L c,f and the Cooper pair breaking does not occur, whereas the condensate of Bose excitations is preserved. The CoE appears in the second-order phase transition. The mother condensate decreases and vanishes at v = v c2 (T ), then the superfluidity is destroyed in a first-order phase transition with an energy release.