A new blow up criterion for the 3D magneto-micropolar fluid flows without magnetic diffusion

This note obtains a new regularity criterion for the three-dimensional magneto-micropolar fluid flows in terms of one velocity component and the gradient field of the magnetic field. The authors prove that the weak solution (u,ω,b)\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$(u,\omega,b)$\end{document} to the magneto-micropolar fluid flows can be extended beyond time t=T\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$t=T$\end{document}, provided if u3∈Lβ(0,T;Lα(R3))\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$u_{3}\in L^{\beta }(0,T;L^{\alpha }(R^{3}))$\end{document} with 2β+3α≤34+12α,α>103\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$\frac{2}{\beta }+\frac{3}{\alpha }\leq \frac{3}{4}+\frac{1}{2\alpha },\alpha > \frac{10}{3}$\end{document} and ∇b∈L4p3(p−2)(0,T;M˙p,q(R3))\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$\nabla b\in L^{\frac{4p}{3(p-2)}}(0,T;\dot{M}_{p,q}(R^{3}))$\end{document} with 1<q≤p<∞\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$1< q\leq p<\infty $\end{document} and p≥3\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$p\geq 3$\end{document}.


Introduction
The aim of this paper is to understand the regularity criterion for the following threedimensional magneto-micropolar fluid flows without magnetic diffusion: (1.1) This system is a special case of the classical three-dimensional magneto-micropolar fluid flows where u = (u 1 , u 2 , u 3 ), ω = (ω 1 , ω 2 , ω 3 ), b = (b 1 , b 2 , b 3 ) and π denote the unknown velocity field, the micro-rotational velocity, the magnetic field and the unknown scalar pressure at the point (x, t) ∈ R 3 × (0, T), respectively. While u 0 , ω 0 , b 0 are the prescribed initial data and div u = div b = 0 in the sense of distributions. The constants μ, χ, κ, γ are positive numbers associated with the properties of the material, where μ is the kinematic viscosity, χ is the vortex viscosity, κ and γ are spin viscosities (more details see [11]). The magneto-micropolar fluid system (1.2) was first proposed by Galdi and Rionero [7]. The existence of global-in-time weak solutions was then established by Rojas-Medar and Boldrini [14], while the local strong solutions and global strong solutions in bounded domain for the small initial data were considered, respectively, by Rojas-Medar [13] and Ortega-Torres and Rojas-Medar [12]. However, whether the local strong solutions can exist globally or the global weak solution is regular and unique is an outstanding open problem. Hence there are many regularity criteria to ensure the smoothness of solutions. Gala [2] proved that, if u ∈ L 2 1-r (0, T;Ṁ p, 3 r (R 3 )) or ∇u ∈ L 2 2-r (0, T;Ṁ p, 3 r (R 3 )), then the local smooth solution (u, ω, b) can be extended beyond t = T. Zhang and Yao [17] When the micro-rotational velocity ω = 0 and χ = 0, Eq. (1.2) becomes the standard magneto-hydrodynamic equations. In recent years, the problem of regularity criteria involving one component has been investigated for the MHD equations (see e.g. [3-5, 8, 9]). In 2016, Yamazaki [15] proved that, if u 3 ∈ L p 0, T; L q R 3 with 2 p + 3 q ≤ 1 3 + 1 2q , 15 2 < q ≤ ∞ and j 3 ∈ L p 0, T; L q R 3 with 2 p + 3 q ≤ 2, 13 2 < q ≤ ∞, then the weak solution (u, b) is regular, where j 3 is the third component of ∇ × b = (j 1 , j 2 , j 3 ). Later Zhang [16] refined the result of Yamazaki's. He proved that, if 15 2 < q ≤ ∞ and j 3 ∈ L p 0, T; L q R 3 with 2 p + 3 q ≤ 2, 3 2 < q ≤ ∞, then the weak solution (u, b) is regular. We further assume that ω = χ = 0, the system (1.1) is usually named MHD equations without magnetic diffusion. In order to present our motivation, we list some information on regularity criteria for 2D-MHD equations without magnetic diffusion. In 2011, Zhou and Fan [18] proved if ∇b ∈ L 1 (0, T; BMO(R 2 )), then the local strong solution (u, b) is regular. Gala, Ragusa and Ye [6] improved Zhou and Fan's result. They showed that, if ∇b ∈ L p p-1 (0, T;Ṁ p,q (R 2 )) with p ≥ q > 1, the local strong solution (u, b) to the MHD equations with magnetic diffusion is regular. Motivated by [2,15], and [6], we will investigate the regularity criterion on the weak solution to the magneto-micropolar flows involving one velocity component and the gradient of magnetic field satisfying (1.3) and (1.4). Our result is stated as follows.
For the two dimension case, due to R 2 u · ∇u · u = 0, the condition ∇b ∈ L 2p p-2 (0, T;Ṁ p,q (R 2 )) is sufficient (see [6]). Compared with the result in [2], due to the magneto-micropolor fluid flows discussed in Theorem 1.1 there is lack of magnetic diffusion, it increases the difficulties of dealing with the nonlinear terms in H 1 -energy estimates, especially for the term R 3 u · ∇w · w dx. Fortunately, the L 3 -energy estimate for ω helps us to overcome these problems.
then the local strong solution (u, b) can be smoothly extended beyond t = T.
Remark 1.2 Comparing with the results either in [15] or in [16], though the MHD equations discussed in Corollary 1.1 show lack of magnetic diffusion and the spatial space of magnetic field is enlightened, it is hard to say our results have refined the one in [15] or that in [16].
The difficulties and strategy are listed as follows: • The first big tiger is to estimate the nonlinear term R 3 u · ∇u · u dx. Since R 3 u · ∇u · u dx = 0, it is impossible to handle it as in the second dimension. We have to present the horizontal energy estimate ∇ h u L 2 , ∇ h b L 2 .
• The second thorn is the nonlinear term R 3 u · ∇w · w dx. Integrating by part gives As usual, if we use the Hölder inequality and the Young inequality, we get which does not work. Thanks to the L 3 -norm estimate of ω and some suitable interpolating inequality, which can be found in Sect. 3, we can overcome these difficulties. More precisely, these methods helps us to handle R 3 u · ∇ω · ω dx and R 3 ∇u · ∇ 2 ω · ω dx successfully. The rest of this paper is organized as follows. The definition of some functional spaces and some useful lemmas are presented in Sect. 2. The L 3 -norm of ω is given in Sect. 3. The proof of Theorem 1.1 is presented in Sect. 4.

Preliminaries and some basic facts
In this section, we will present some information on the Morrey space and introduce the definition of a weak solution to the magneto-micropolar equation (1.1). Definition 2.1 (see [10]) For 1 < q ≤ p ≤ ∞, the homogeneous Morrey space is presented as follows: where B(x, R) denotes the closed ball in R 3 with center x and radius R.
The following lemma plays a crucial role in proving the regularity criterion for the magneto-micropolar fluid flows (1.1). Lemma 2.1 (see [10]) (1) Let 1 < p ≤ q < ∞ and p, q such that 1 The Sobolev-Ladyzhenskaya inequality in the whole space R 3 reads as follows.
Lemma 2.2 (see [1]) There exists a constant C > 0 such that for every φ ∈ H 1 (R 3 ) and every p ∈ [2,6], where C is a constant depending only on p.
The definition of a weak solution to the magnetic micropolar equation is provided in the following.

Some useful lemmas
The following L 3 -energy estimate is needed to prove our result. Then
Proof Multiplying (1.1) 2 by |ω|ω and integrating over R 3 , we have where we have used To estimate the nonlinear term on the right hand side, integrating by parts and using the Young inequality and (4.1), we obtain Substituting the above inequality into (3.2) gives Integrating on [0, t) and using (4.1) yield

Proof of Theorem 1.1
In this section, we shall give the proof of Theorem 1.1. We will assume that μ = χ = γ = κ = 1 throughout this paper. Let [0, T * ) be the maximal time interval for the existence of the local smooth solution. If T * ≥ T, the conclusion is obviously valid, but for T * < T, we would show that under the assumption of (1.3) and (1.4). Hence, according to the definition of T * , this leads to a contradiction.
Step 1: L 2 -energy estimate A standard energy method says (4.1) Step 2: H 1 -Horizontal energy estimate We first establish the horizontal gradient of the velocity u and magnetic field b. Taking ∇ h on both sides of Eqs. (1.1) 1 and (1.1) 3 , multiplying by ∇ h u and ∇ h b, respectively, and integrating over R 3 , we get We start to estimate A 2 . From (1.1) 4 and Lemma 2.1 and the fact ∇ · u = ∇ · b = 0, we know that (p ≥ 3) Thanks to the Hölder and Young inequalities, one deduces Now it is time to deal with the first term A 1 . Integrating by parts, we get (4.5) Using integration by parts again and applying the fact that div u = 0, it yields and Substituting (4.6) and (4.7) into (4.5) yields Thanks to the Hölder inequality, (2.1) and the Young inequality, we obtain for α > 3 (4.10) Integrating over [0, t) and using (4.1), one can verify (4.11) Step 3: H 1 -full energy estimate Multiplying (1.1) 1 , (1.1) 2 and (1.1) 3 byu,ω andb, respectively, and integrating over R 3 , then adding them we obtain where we have used the inequalities Now, we estimate B 2 , B 5 and B 6 . After applying integration by parts, div u = div b = 0, the Hölder inequality, Lemma 2.1, the Sobolev interpolation inequality and the Young inequality, we have (4.13) We can infer from the Hölder and the Young inequalities that (4.14) Applying integration by parts we obtain Thanks to the Hölder inequality, the interpolation inequality with 3 ≤ α ≤ 9 and Lemma 3.1, we arrive at (4.16) Similarly, the term B 32 can be bounded as follows: (4.17) For the term B 1 , similar to A 1 , we find that Combining (4.13), (4.14), (4.16), (4.17) and (4.18), then (4.12) becomes Integrating over [0, t] yields where We proceed to estimate G(t). From (4.1) and (4.11), we deduce that ≤ C ∇ h u 0