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tokens: which is proposed and numerically simulated in two dimensions (2D), and 3D (Heyvaerts et al. 1977 ; Shibata et al. 1992 ; Yokoyama Shibata 1995 , 1996 ; Shimojo et al. 1996 ; Nishizuka et al. 2008 ; Pariat et al. 2009 ). In this model, the closed magnetic arch emerges into the ambient unipolar field and then reconnection occurs between the unipolar field and one branch of the arch with an opposite polarity to the unipolar field. The other is the blowout model (Moore et al. 2010 , 2013 ) with two magnetic reconnection processes. The first magnetic reconnection, which is similar to that in the standard model, occurs between the emerging magnetic arch and the ambient unipolar field. Then a filament with a large amount of pent-up free energy by shear (or twist) dominates the second magnetic reconnection (Liu et al. 2011a , 2011b ; Moreno-Insertis Galsgaard 2013 ; Hong et al. 2014 ; Lee et al. 2015 ). Recently, Sterling et al. ( 2015 ) suggested that all of the jets in the coronal hole essentially come from mini-filament eruptions. According to the latest review (Raouafi et al. 2016 ), the standard jets are intensively collimated, usually form an inverse-Y shape with a narrow spire, and seldom rotate. However, the blowout jets strongly rotate and posses a relatively broad spire. As suggested by Pariat et al. ( 2010 ), a jet process is always dominated by a synthetic role from magnetic geometrical characteristics of the jet source, such as size, flux distribution, null point position, and asymmetry. Many observations find that jets could appear with similar morphology and outflow, but might possess distinctive magnetic structures in the low coronal source region (Nisticò et al. 2009 ; Zhang et al. 2012 ). In total, a large number of observations and theoretical models basically describe and explain the morphology, dynamical and physical properties of the jets. However, for the limitation of observational capability, there is no appreciable resolution to distinctly resolve the motions of the plasma blobs (Zhang Ji 2014b ) and the related variation of magnetic topological structure inside a jet. Fortunately, benefitting from the extremely high spatial and temporal resolution in special wavelength observations by the Interface Region Imaging Spectrograph ( IRIS ; De Pontieu et al. 2014 ) and all ultraviolet (UV) and EUV wavelengths of the Atmosphere Imaging Assembly (AIA; Lemen et al. 2012 ) on board the Solar Dynamics Observatory ( SDO ; Pesnell et al. 2012 ), a cusp-shaped structure jet was captured with unprecedented detailed observations. The formation and evolution processes of the jet, including the motions of the blobs and topological variation of its skeleton, are described in Section 2 . Section 3 contains a discussion and conclusions. 2. OBSERVATIONS 2.1. Data From 05:51 UT to 06:39 UT on 2014 August 29, IRIS narrow-band slit-jaw images (SJIs; see Figure 1 ) in the 1330 Å channel captured a cusp-shaped jet located at N08W90 (Solar-X: