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The Majorana representation for generalized GHZ states |gGHZ ≡ a|000 + b|111, and generalized W states |gW ≡ c|001 + d|010 + e|100. Here, a ≡ cos ϑ, b ≡ sin ϑ, and ϑ = π/10.

The Majorana representation for generalized GHZ states |gGHZ ≡ a|000 + b|111, and generalized W states |gW ≡ c|001 + d|010 + e|100. Here, a ≡ cos ϑ, b ≡ sin ϑ, and ϑ = π/10.

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Majorana stars, the 2j spin coherent states that are orthogonal to a spin-j state, offer a visualization of general quantum states and may disclose deep structures in quantum states and their evolutions. In particular, the genuine tripartite entanglement—the three-tangle of a symmetric three-qubit state, which can be mapped to a spin-3/2 state—is m...

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... to the equator-the closer to the equator, the higher the entanglement. As an example, a generalized Greenberger-Horne-Zeilinger (GHZ) state |gGHZ ≡ a|000 + b|111 with a three-tangle 4a 2 b 2 is already symmetrized and hence is represented by three distinct Majorana stars distributed evenly on the southern hemisphere with the same latitude [see Fig. ...
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... root. Hence, a generalized W state is represented by three Majorana stars on unit sphere-one is located at the south pole and two degenerate ones are located at the north pole. It shows that the appearance of a pair of degenerate Majorana stars on the unit sphere indicates the vanishing of the three-tangle for a general three-qubit state [see Fig. ...

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... Apart from indisputable mathematical advantages [22], this picture builds a bridge between the abstract Hilbert space (where the states live) and the simple geometry of the Bloch sphere. Consequently, this representation rapidly meets the increasing interest in high-dimensional quantum systems and, several decades after its conception, is being used in fields as diverse as polarization [23][24][25][26][27], spinor Bose gases [28][29][30][31], multiqubit systems [32][33][34][35][36][37][38], metrology [39][40][41][42][43], geometric phases [44][45][46][47][48][49][50][51], non-Hermitian lattices [52], and algebraic quantum models such as the Lipkin-Meshkov-Glick model [53,54]. The distribution of Majorana stars conveys complete information and can be directly computed when the quantum state is known. ...
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... However, the problem of creating analogues of more general entanglements in classical continuum systems continues to present challenges [10,17,18]. Here, by building on ideas underlying the Poincaré-Bloch sphere [19,20] and Majorana star [21][22][23][24] representations of quantum states, we exhibit a family of formal mappings between n-qubit states and 2D hydrodynamic flow fields. The topological defects and stagnation points of these flow fields encode properties of the corresponding n-qubit state. ...
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... These 2J points are called Majorana stars (MSs) of the state. Consequently, this representation becomes an efficient method to study the geometric related properties of multipartite or high-dimensional state such as entanglement [2][3][4][5][6][7][8][9][10][11], Berry phase [12][13][14][15][16][17][18], as well as their dynamics, geometric structures and response to geometric transformations (e.g. rotations and inversions) [19][20][21][22][23][24][25][26][27][28][29]. ...
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... We define the distance between two Majorana points as η = cos −1 (Ŝ 1 .Ŝ 2 ) = cos −1 [sin θ 1 sin θ 2 cos(ϕ 1 − ϕ 2 ) + cos θ 1 cos θ 2 ], where the Majorana starsŜ k have respective spherical coordinates (θ k , ϕ k ), k ∈ {1, 2}. This distance can be interpreted as a direct measure of entanglement between two qubits in the symmetrized-state representation of the qutrit [14,15]. Explicitly, any spin-1 state -and, by the identification above, any qutrit state Eq. ...
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We show that stimulated Raman adiabatic passage (STIRAP) and its superadiabatic version (saSTIRAP) have a natural geometric two-star representation on the Majorana sphere. In the case of STIRAP, we find that the evolution is confined to a vertical plane. A faster evolution can be achieved in the saSTIRAP protocol, which employs a counterdiabatic Hamiltonian to nullify the non-adiabatic excitations. We observe how, under realistic experimental parameters, the counterdiabatic term corrects the trajectory of the Majorana stars toward the dark state. We also introduce a spin-1 average vector and present its evolution during the two processes. We show that the Majorana representation can be used as a sensitive tool for the detection of process errors due to ac Stark shifts and non-adiabatic transitions.
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