在重力的波因卡瑞規範理論中僅存的兩種行為良好的動力聯絡模式
分別為：spin-0+ 及spin-0-。 我們分別在兩種宇宙模型之下研究
此兩種模式的動力特性。這兩種動態純量的扭稱模式所產生的效應
可以用來解釋加速膨脹宇宙的現象。我們經由數值模擬的方式檢驗
在近期漸進的範圍內的動力演化（近似對應到目前的宇宙）； 在此
案例中顯現出兩種動力扭稱模式為分立的，而宇宙加速膨脹的現象
僅由spin-0+ 模式所決定。目前有一更一般化的BHN模型被提出探
討。我們也研究了明顯各向同性的Bianchi 宇宙模型。我們也研究
了A類第一及第九型與B類第五型的動力方程式，可以顯示出等效
的拉格朗日量與漢米爾頓量可以良好的運作。我們也重新審視物質
自旋密度在扭稱宇宙學中所扮演的角色，我們認為自旋密度並沒有
直接驅動此種動力純量模式。

In the Poincar''e gauge theory of gravity only two modes with well behaved dynamics have been found. They are effectively scalar modes, carrying spin-0+and spin-0-. We have investigated the dynamics of these modes in some cosmological models.
The effects these two
dynamic scalar torsion could account for the presently
accelerating universe. We had examined via numerical simulation the late time
asymptotic regime of the dynamical evolution (approximately corresponding to our current Universe); in that case
it turns out that the two dynamic torsion modes decouple, and the acceleration of the
Universe is determined only by the spin-0+ mode.
Now a more general ansatz in the framework of
BHN PG model has been proposed. Rather than use a FLRW representation we have used a manifestly homogeneous Bianchi representation. The effective Lagrangian and Hamiltonian
form of the dynamic equations for this model has been found for the isotropic Bianchi class A (type I, IX) and class B (type V) cosmologies.
The role of the material spin density in torsion cosmology has been reconsidered,
we argue that that the spin density does not directly drive the dynamic scalar modes.

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