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As a general rule, we can use the majority-minority splitting from GW to estimate U for partially occupied d orbitals in other TBrPP- M (M=transition metal-atom) compounds. The strength of U depends crucially on the total magnetization of the molecule (TBrPP-Mn, for instance, has values of U several eVs larger than TBrPP-Co) and on the strength of the TBrPP molecular field.
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As a general rule, we can use the majority-minority splitting from GW to estimate U for partially occupied d orbitals in other TBrPP- M (M=transition metal-atom) compounds. The strength of U depends crucially on the total magnetization of the molecule (TBrPP-Mn, for instance, has values of U several eVs larger than TBrPP-Co) and on the strength of the TBrPP molecular field.
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The HOMO-1, HOMO-2, and HOMO-3 orbitals, although closer in energy to EF than 3 d z2, are localized further away from the center of the molecule level, with a high amplitude on the phenyl-bromine radicals. Thus, their contribution to the STM signal with the tip placed on top of the Co atom is negligible.
-
The HOMO-1, HOMO-2, and HOMO-3 orbitals, although closer in energy to EF than 3 d z2, are localized further away from the center of the molecule level, with a high amplitude on the phenyl-bromine radicals. Thus, their contribution to the STM signal with the tip placed on top of the Co atom is negligible.
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In this approximation, we are neglecting many-body contributions due to the Coulomb interactions between the electrons in orbital i entering the model (e.g., cobalt d3 z2 -1 electrons) and the electrons in the surface. Such contributions are likely to be much smaller than the interaction effects of electrons within orbital i, which are well captured by the GW calculation in vacuum.
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In this approximation, we are neglecting many-body contributions due to the Coulomb interactions between the electrons in orbital i entering the model (e.g., cobalt d3 z2 -1 electrons) and the electrons in the surface. Such contributions are likely to be much smaller than the interaction effects of electrons within orbital i, which are well captured by the GW calculation in vacuum.
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