本文選題：quintessence + holographic�。� 參考：《Communications in Theoretical Physics》2014年06期

【摘要】：In this paper we consider quintessence reconstruction of interacting holographic dark energy in a non-flat background. As system's IR cutoff we choose the radius of the event horizon measured on the sphere of the horizon,defined as L = ar(t). To this end we construct a quintessence model by a real, single scalar field. Evolution of the potential, V(φ), as well as the dynamics of the scalar field, φ, is obtained according to the respective holographic dark energy. The reconstructed potentials show a cosmological constant behavior for the present time. We constrain the model parameters in a flat universe by using the observational data, and applying the Monte Carlo Markov chain simulation. We obtain the best fit values of the holographic dark energy model and the interacting parameters as c = 1.0576+0.3010+0.3052-0.6632-0.6632and ζ = 0.2433+0.6373+0.6373-0.2251-0.2251, respectively. From the data fitting results we also find that the model can cross the phantom line in the present universe where the best fit value of the dark energy equation of state is wD=-1.2429.
[Abstract]:In this paper we consider quintessence reconstruction of interacting holographic dark energy in a non-flat background. As system's IR cutoff we choose the radius of the event horizon measured on the sphere of the cutoff we choose the radius of the event horizon measured on the sphere of the defined as L = Artemia. To this end we construct a quintessence model by a real, single scalar field. Evolution of the potential, V (蠁 O, as well as the dynamics of the scalar field, 蠁, is obtained according to the respective holographic dark energy.) The reconstructed potentials show a cosmological constant behavior for the present time. We constrain the model parameters in a flat universe by using the observational data, and applying the Monte Carlo Markov chain simulation. We obtain the best fit values of the holographic dark energy model and the interacting parameters as c = 1.0576 0.3010 0.3052-0.6632-0.6632and 味 = 0.2433 0.6373 0.6373-0.2251-0.2251, respectively. From the data fitting results we also find that the model can cross the phantom line in the present universe where the best fit value of the dark energy equation of state is wD- 1.2429.
【作者單位】： Physics
【基金】：supported financially by Research Institute for Astronomy & Astrophysics of Maragha (RIAAM), Iran
【分類號(hào)】：P159

【參考文獻(xiàn)】

相關(guān)期刊論文 前1條

1 萬里川,周建光,李杰之,孫玉龍;外源高表達(dá)PC-1蛋白N端43個(gè)氨基酸可加速人前列腺癌細(xì)胞系C4-2的生長[J];生物技術(shù)通訊;2004年01期

【共引文獻(xiàn)】

相關(guān)期刊論文 前5條

1 M.Sharif;Sehrish Azeem;;Dark Energy Models and Cosmic Acceleration with Anisotropic Universe in f(T) Gravity[J];Communications in Theoretical Physics;2014年04期

2 周立權(quán),張惠,高雪松,王健,梁瑞霞,洪寶發(fā),周建光;RNA干涉抑制NIH3T3細(xì)胞中外源PC-1基因表達(dá)[J];軍事醫(yī)學(xué)科學(xué)院院刊;2005年01期

3 周立權(quán),張惠,高雪松,王健,梁瑞霞,洪寶發(fā),周建光;RNA干涉技術(shù)穩(wěn)定抑制PC-1基因表達(dá)對(duì)前列腺癌細(xì)胞C4-2的影響[J];中華男科學(xué)雜志;2005年04期

4 ZHANG JingFei;ZHAO LiAng;ZHANG Xin;;Revisiting the interacting model of new agegraphic dark energy[J];Science China(Physics,Mechanics & Astronomy);2014年02期

5 Farzin Adabi;Kayoomars Karami;Fereshte Felegary;Zohre Azarmi;;Interacting viscous entropy-corrected holographic scalar field models of dark energy with time-varying G in modified FRW cosmology[J];Research in Astronomy and Astrophysics;2012年01期

相關(guān)博士學(xué)位論文 前2條

1 黃鵬;暗能量與f（T）引力相關(guān)問題研究[D];北京工業(yè)大學(xué);2013年

2 王鈺婷;暗能量的擾動(dòng)和積分的Sachs-Wolfe效應(yīng)[D];大連理工大學(xué);2013年

相關(guān)碩士學(xué)位論文 前4條

1 潘文劍;全息暗能量模型與宇宙空間演生現(xiàn)象的研究[D];南昌大學(xué);2013年

2 張欣;Horava-Lifshitz引力理論的熱力學(xué)行為以及全息暗能量的熱力學(xué)描述[D];遼寧師范大學(xué);2013年

3 韓偉麗;關(guān)于加速膨脹宇宙中f（R）引力模型構(gòu)建的研究[D];遼寧師范大學(xué);2013年

4 林亮亮;關(guān)于f（R，，L_m）引力理論及其相關(guān)問題的研究[D];遼寧師范大學(xué);2013年

【二級(jí)參考文獻(xiàn)】

相關(guān)期刊論文 前1條

1 王健,周建光,李杰之,張浩,陳珊,黃翠芬;PC-1基因在腫瘤組織中的表達(dá)及其啟動(dòng)子區(qū)的克隆和活性分析[J];癌癥;2002年11期

本文編號(hào)：2042405