IS PULSAR B0628-28 REALLY AN EXCEPTION?. Cuilan Qiao Mentor:Pro. Xiangdong Li Dec.7, 2005. OUTLINE. 1 Introduction 2 Data analysis for spin-powered pulsars 3 Theoretic discussion 4 Conclusion. 1 Introduction. Observation of pulsar B6028-28 Chandra:
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Mentor:Pro. Xiangdong Li
► Was observed twice:first on Nov.4,2001 and again on 2002 Mar.25 for 2000 and 17000s respectively;1.141s exposures.
► position is
► Was observed on 2004 Feb. 28 for a total on time of 48ks;47ks exposures.
► position is
► The longest period radio pulsar detected in X-rays (P=1244ms).
► The Chandra data yielded a luminosity 2 orders of magnitude greater than what is expected for a spin-powered pulsar(logLx=30.34).
From Tepedelenlioglu et. al ,APJ astro-ph/0505461
► Zscore-----data standardization
► Pdist-----calculate space between two objects by Euclidean distance
► Squareform-----Euclidean distance matrix
► Linkage-----nearest neighbor method
► cluster-----cluster data
► find----- find elements of every group
► Dendrogram-----draw clustering graph
The basic simplification is that the emitting region can he treated as one zone
One-zone model that does not attemp to account for the spatial structrue of the nebulae.