Received 7 January 2016; accepted 3 May 2016; published 6 May 2016
Canonical Lagrangian has been studied in the context of classical mechanics, quantum field theory and other branches of physics. The standard form of canonical Lagrangian density is given by
Here and also action S is dimensionless then, Lagrangian density has dimension of and hence dimension of is M (here M stands for mass). Also we are considering the case of one time and one space dimension. Thus, where corresponds to time coordinate t, and corresponds to space coordinate x. Here the metric tensor is diagonal, and is given by
In this framework, Lagrangian density (1) can be written as
Here kinetic energy term is quadratic. Lagrangian density (1) has been extensively studied in the context of quantum field theory, theory of phase transition and other branches of physics  -  . In recent years, non canonical Lagrangian density has been used in the inflationary cosmological models  -  (see ref.  for further details). In the context of cosmological model, even in absence of any potential energy term, a general class of non-standard (i.e., non-quadratic) kinetic energy terms, for a scalar field, can drive an inflationary evolution of the same type as the usually considered potential driven inflation. The mathematical form of non canonical Lagrangian density is given by the following equation:
where is the potential and n is an integer. For, we get the usual Lagrangian of the scalar field theory. Also, note that the Equation (4) is Lorentz invariant for any value of n. The purpose of this work is to obtain the exact solution of Equation (4) in (1 + 1)-dimension for, and for the different potentials. For, Equation (4) takes the form
Also, we are using natural units in which and action is dimensionless. In this unit is dimensionless. The corresponding equation of motion is given by
Thus the Lagrangian density is given by
From here one can see that the kinetic energy is non-quadratic and that’s why the Lagrangian is known as non-canonical Lagrangian. The corresponding equation of motion is given by
Here represents the time derivative of field and represents the spatial derivative. Note that the equation of motion remain second order. Also, for a Lorentz invariant system once a static solution is known, moving solutions are obtained by transforming to a moving coordinate system  (we are interested in solitary and periodic wave solutions). Now for static case, the equation of motion becomes
Multiplying both sides by and integrating with respect to x, we obtain
where C is constant of integration. Let and vanishes at and hence. Thus finally we obtain
For in Equation (4), the corresponding equation of motion is given by
In the next section we will solve Equation (11) for some specific potentials. Also, Equation (11) cannot be solved for every potential. We will consider only those potentials for which Equation (11) can be integrated.
In this section we are going to solve Equation (11) for the following potentials.
Case I: Let us first consider the potential
where is real constant and its dimension is. This potential is used in the theory of phase transition and is taken from reference  . For this potential, Equation (11) takes the form
After integrating this equation, we obtain
where is constant of integration. To solve the left hand integral, we substitute and after solving this integral, we obtain
For time dependent case, the corresponding solution can be obtained by Lorentz transformation
From this solution one can see that, for we obtain periodic solution and for, we obtain hyperbolic solution. The hyperbolic solution diverges for large x and t. Now the energy of the field is given by
where is energy density and is given by
where is momentum density and is time derivative of the field. Here
where is spatial derivative of the field. Using Equations ((20) and (21)), we obtain
For static case, we obtain
Using Equation (11), we get
Note that, otherwise energy density becomes imaginary. The total energy is given by
For time dependent case, energy density is given by
For, and for the given potential Equation (16), we obtain from Equation (12) the following solution
which is a kink solitary wave solution  for. Thus in this case solution exist for. Energy density in this case is given by
The energy density is localised near. According to the definition of  , localised solutions are those solutions to the field equation whose energy density at any finite time t is localised in space and falls to zero at spatial infinity.
Case II: Here we will consider the potential of the form
In this case, the solution of time independent field equation is given by
Note that this solution is a solitary wave solution for. Similarly, the corresponding solution of time dependent case is given by
The energy density of time independent case is given by
and the energy density of time dependent case is given by
Thus the energy density is localised.
3. Concluding Remarks
In this work we have discussed the non-canonical lagrangian for different kinds of potential. We have obtained the periodic and solitary wave solutions. A comparison is also made between the solutions of canonical and non-canonical lagrangian. As one can see that for Equation (16), the solution exists only when whereas, for the same potential and for canonical Lagrangian, the solution exists for. Also the solution of non- canonical lagrangian is periodic and canonical lagrangian admits the solitary wave solution. Similarly for the potential (32), the non-canonical lagrangian admits the solitary wave solution for. Although non-canonical Lagrangian has been used in the inflationary model, the result obtained in this work may be used to explain the phenomena of phase transition and other quantum field theoretic model.
We would like to thank Sanil Unnikrishnan for helpful discussions.
 Khare, A. and Saxena, A. (2006) Domain Wall and Periodic Solutions of Coupled 4 Models in an External Field. Journal of Mathematical Physics, 47, Article ID: 092902. http://dx.doi.org/10.1063/1.2345110
 Unnikrishnan, S., Sahni, V. and Toporensky, A. (2012) Refining Inflation Using Non-Canonical Scalars. Journal of Cosmology and Astroparticle Physics, 2012, 018. http://dx.doi.org/10.1088/1475-7516/2012/08/018