黑洞时空中的quintessence效应

The effect of quintessence in black hole spacetime

引进了一个研究时空分类的新方法,并在充满quintessence的RN(A)dS (Q-RN(A)dS)时空中,研究了时空的视界和粒子的测地线.我们发现非极端的Q-RNAdS时空存在两类黑洞,一类有2个视界,另一类有4个视界.在束缚态的情况下,有质量粒子在有两个视界的时空中,其测地线随quintessence参数r_q增大(即暗能量的影响减小)每个周期远日点(或近日点)的进动角度增大;而随着态方程参数w_q的减小,运动一周到达远日点(或近日点)次数增多,这表明人们可以根据进动角度和到达远日点的次数确定参数r_q和w_q的取值范围.对于非极端的Q-RNdS度规,时空也分为两类,一类是只有1个宇宙视界的类de Sitter时空,另一类的时空有3个视界,其中一个为宇宙视界,另外两个分别为黑洞内、外视界.有趣的是,类de Sitter时空中心是一个裸奇点,但是任何粒子不可能到达裸奇点,因为此处的有效势趋于无穷大.在束缚态的情况下,粒子在这种时空中运动的轨迹受暗能量的影响不显著.值得指出的是,在具有4个视界的Q-RNAdS时空和3个视界的Q-RNdS时空中运动的粒子不存在束缚态.

A new method is introduced to study the classification of spacetime, and spacetime horizons and timelike geodesics are investigated in the background spacetime of Reissner-Nordstrrm-（anti-）de Sitter black hole surrounded by the quintessence （Q-RN（A）dS）. We find that, for Q-RNAdS metric, there are two types of black holes： two horizons and four horizons. In a black hole spacetime of two horizons, the angular precession of the aphelion per revolution increases with the increase of the quintessence parameter rq; while the number of aphelion per revolution increases with the decrease of the quintessence equation of state parameter Wq. This shows that the quintessence parameters rq and Wq can be determined by measuring the angular precession and number of aphelion per revolution, respectively. For Q-RNdS metric there are two cases： one horizon and three horizons. The Q-RNdS metric of one horizon describes the de Sitter-like spacetime, which has a naked singularity at r = 0. It is interesting to note that any particle never reaches the singularity, since the effective potential is infinite at the point. On the other hand, the quintessence has no significant on the geodesics in de Sitter-like spacetime. It is worth pointing out that there are no bound states for the Q-RNAdS spacetime with four horizons and the Q-RNdS spacetime with three horizons.