论文标题
k essence古典汉密尔顿方法，用于加速宇宙的扩展，$ω\ of Yout-1 $
k-essence classical Hamiltonian approach for an accelerated expansion of the Universe with $ω\approx-1$
论文作者
论文摘要
我们获得了$ k $ - essence scalial field $ ϕ（r，t）$的拉格朗日，带标量曲率$ k $的Friedmann-Lemaitre-Robertson-Walker（FLRW）Metric。获得的Lagrangian具有两个广义的坐标$ ϕ $和比例因子的对数（$ q = \ ln a $）。经典的Hamiltonian $（{\ Mathcal H}）$是根据两个相应的共轭动量$ p_ {q} $和$ p_ϕ $获得的。解决汉密尔顿运动方程，我们获得了比例因子$ a（t）$，能量密度$ρ$的经典解决方案，状态参数$ω$和减速参数$ q_ {0} $。在$ t \ rightArrow \ infty $的最晚时间，我们有时间缩放因子随时间的指数增长，能量密度$ρ$变为恒定，我们可以将其识别为黑暗能量密度，状态参数方程将变为$ω\ -1 $，减速参数变为$ q_ {0} {0} {0} \ oft -1 $。所有这些结果表明，由称为暗能量的负压驱动的宇宙的膨胀加速。
We obtain lagrangian for $k$-essence scalar field $ϕ(r,t)$ with scalar curvature $k$ of Friedmann-Lemaitre-Robertson-Walker (FLRW) metric . Obtained lagrangian has two generalised co-ordinates $ϕ$ and logarithm of scale factor ($q=\ln a$). Classical Hamiltonian $({\mathcal H})$ is obtained in terms of two corresponding conjugate momentum $p_{q}$ and $p_ϕ$. Solving Hamilton's equation of motion , we obtain classical solution for scale factor $a(t)$, energy density $ρ$, equation of state parameter $ω$ and deceleration parameter $q_{0}$ . At late time as $t\rightarrow\infty$, we have an exponential growth of scale factor with time, energy density $ρ$ becomes constant, which we can identify as dark energy density, equation of state parameter becomes $ω\approx -1$ and deceleration parameter becomes $ q_{0}\approx -1$. All this results indicates an accelerated expansion of universe driven by negative pressure known as dark energy.
