我們利用擬合X 射線連續光譜方法去限制 X 射線雙星GX 339-4 中的恆星級黑洞的自旋。Reis et al. (2008) 利用鐵K α 線模型測定出它的自旋為a*=0.935±0.01。然而，Kolehmainen & Done (2010)從X 射線連續光譜中得到它的自旋不會超過0.9 的結果。為了解決這兩個不一致的結果並計算其自旋，我們先採用兩個相對論性吸積薄盤模型，並且結合簡單的康普吞化模型，用以擬合RXTE/PCA 對於GX 339-4 自2002 年至2010 年的爆發觀測的X 射線連續光譜。我們依循McClintock et al. (2006) and Steiner et al. (2009a & 2010)的建議，為了利於進一步分析而設立了限制條件以挑選符合吸積薄盤模型的資料。我們更進一步地利用新建立的修正模型(McClintock et al. 2006)去限制這黑洞的自旋。我們的結果顯示這個黑洞的自旋不會超過a*=0.94，這似乎支持了Reis et al. (2008)的結果。 We present our analysis result for constraining the spin of the stellar-mass black hole (BH) in the X-ray binary GX 339-4 by fitting its X-ray continuum spectra. Reis et al. (2008) determined its spin to be a*=0.935±0.01 by modeling the profile of Fe K α line. However, Kolehmainen & Done (2010) concluded that its spin is no more than 0.9 from X-ray continuum fitting method. To resolve these contradictive results and estimate its spin, we first adopted two fully relativistic, thin accretion disk models combined with a simple comptonization model to fit X-ray continuum spectra of GX 339-4 observed by Proportional Counter Array (PCA) on Rossi X-Ray Timing Explorer(RXTE) during its 2002-2010 outbursts. We set up constraints suggested by McClintock et al. (2006) and Steiner et al. (2009a & 2010) to select the data suitable for thin accretion disk model to further analyze. We then used the most recently developed modified model (McClintock et al. 2006) to further constrain the black hole spin. Our result indicates that the BH spin is no less than a*=0.94, which is likely favorable to the result from Reis et al. (2008).
