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Small indium-doped carbon clusters InCn+(n=110) are systematically studied by the density functional theory at the B3 LYP/LANL2 DZ level. The computed properties include equilibrium geometries, electronic energies, vibrational frequencies, dipole moments and rotational constants for individual species. The calculation results show that the open-chain linear isomers with the indium atom bound to the end of the carbon chain are the most stable geometry in all cases. There must exist a cyclic or fan structure in the metastable or the third stable structure of cluster. The bigger the size of the cluster, the more obvious the stability of the structure is. The electronic ground state is found to be alternately a triplet for even n and a singlet for odd n with the only exception of InC+. It is generally observed that the spin contamination is not serious for all electronic ground states because the s2 values are uniform and in general deviate slightly from the pure spin values, and the B3 LYP wave functions are nearly spin-pure. It is also found that in the lowest-energy linear structure, the InC bond is longer (from 2.319 to 2.850 ) than the corresponding CC bonds in a range from 1.268 to 1.360 . The CC distances can be assimilated to moderately strong double bonds underlying a clear bonding in the corresponding structures. In addition, we observe a clear alternation in CC distances. The CoddCeven distances are shorter than the CevenCodd ones which mainly results from the charge distribution and spin density. According to the calculation and analysis of the incremental binding energy and the second difference we can deduce an even-odd alternation in the cluster stability for the linear InCn+, with their n-odd members being more stable than the adjacent even-numbered ones. This parity effect also appears in the adiabatic ionization potential curves. The analysis of magnetic properties shows the even-odd alternation with n-even clusters presenting higher values of magnetic moment than n-odd ones. The study of the polarizability indicates that the average values of both the polarization tensors and the anisotropic invariants increase with the size of cluster increasing.
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Keywords:
- density functional theory /
- stability /
- magnetic property /
- polarizability
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[12] Liang J X, Zhang C 2010 Acta Chim. Sin. 68 7
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[16] Largo A, Redondo P, Barriento S 2002 J. Phys. Chem. A 106 4217
[17] Li G L, Tang Z C 2003 J. Phys. Chem. A 107 5317
[18] Chertihin G V, Andrews L, Taylor P R 1994 J. Am. Chem. Soc. 116 3513
[19] Zhang C J, Jiang Z Y, Wang Y L 2013 Comput. Theor. Chem. 1004 12
[20] Wadt W R, Hay P J 1985 J. Chem. Phys. 82 284
[21] Jia L C, Zhao R N, Han J G, Sheng L S, Cai W P 2008 J. Phys. Chem. A 112 4375
[22] Li G L, Xing X P, Tang Z C 2003 J. Chem. Phys. 118 6884
[23] Qi J Y, Dang L, Chen M D, Wu W, Zhang Q E, Au C T 2008 J. Phys. Chem. A 112 12456
[24] Li G L, Wang C Y 2007 J. Mol. Struct. 824 48
[25] Wang L J, Zhang C J, Wu H S 2005 Acta Phys. Chim. Sin. 21 244(in Chinese) [王利江, 张聪杰, 武海顺 2005 物理化学学报 21 244]
[26] Ma W J, Song X, Zhang X M, Wu H S 2010 Acta Phys. Chim. Sin. 26 1396(in Chinese) [马文瑾, 宋翔, 张献明, 武海顺 2010 物理化学学报 26 1396]
[27] Cheng L J 2012 J.Chem. Phys. 136 104301
[28] Cheng L J, Yang J L 2013 J. Chem. Phys. 138 141101
[29] Li L F, Cheng L J 2013 J. Chem. Phys. 138 094312
[30] Feng Y Q, Cheng L J 2015 RSC Adv. 5 62543
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[1] Pauzat F, Ellinger Y 1989 Astron. Astrophys. 216 305
[2] Maccarthy M T, Kalmus P, Gottlieb C A 1996 Astrophysics 467 125
[3] Cernicharo J, Guelin M 1996 Astron. Astrophysics 309 27
[4] Guelin M, Cernicharo J, Travers M J 1997 Astrophysics 37 1
[5] Schermann G, Grosser T, Hampel F 1997 Chem. Eur. J. 3 1105
[6] Dembinski R, Bartik T, Bartik B 2000 J. Am. Chem. Soc. 122 10
[7] Becker S, Dietze H 1988 Int. J. Mass Spectrom. 82 287
[8] Consalvo D, Mele A, Stranges D 1989 Int. J. Mass Spectrom. 91 319
[9] Liu Z Y, Wang C R, Huang R B 1995 Int. J. Mass Spectrom. 141 201
[10] Liu Z Y, Huang R B, Tang Z C 1998 J. Chem. Phys. 229 335
[11] Chuchev K, BelBruno J J 2004 J. Phys. Chem. 108 5226
[12] Liang J X, Zhang C 2010 Acta Chim. Sin. 68 7
[13] Wang C R, Huang R B, Liu Z Y 1995 Chem. Phys. Lett. 242 55
[14] Nakajima A, Taguwa T, Nakao K 1995 J. Chem. Phys. 103 2050
[15] Pascoli G, Lavendy H 2002 Opt. Plasma Phys. 19 339
[16] Largo A, Redondo P, Barriento S 2002 J. Phys. Chem. A 106 4217
[17] Li G L, Tang Z C 2003 J. Phys. Chem. A 107 5317
[18] Chertihin G V, Andrews L, Taylor P R 1994 J. Am. Chem. Soc. 116 3513
[19] Zhang C J, Jiang Z Y, Wang Y L 2013 Comput. Theor. Chem. 1004 12
[20] Wadt W R, Hay P J 1985 J. Chem. Phys. 82 284
[21] Jia L C, Zhao R N, Han J G, Sheng L S, Cai W P 2008 J. Phys. Chem. A 112 4375
[22] Li G L, Xing X P, Tang Z C 2003 J. Chem. Phys. 118 6884
[23] Qi J Y, Dang L, Chen M D, Wu W, Zhang Q E, Au C T 2008 J. Phys. Chem. A 112 12456
[24] Li G L, Wang C Y 2007 J. Mol. Struct. 824 48
[25] Wang L J, Zhang C J, Wu H S 2005 Acta Phys. Chim. Sin. 21 244(in Chinese) [王利江, 张聪杰, 武海顺 2005 物理化学学报 21 244]
[26] Ma W J, Song X, Zhang X M, Wu H S 2010 Acta Phys. Chim. Sin. 26 1396(in Chinese) [马文瑾, 宋翔, 张献明, 武海顺 2010 物理化学学报 26 1396]
[27] Cheng L J 2012 J.Chem. Phys. 136 104301
[28] Cheng L J, Yang J L 2013 J. Chem. Phys. 138 141101
[29] Li L F, Cheng L J 2013 J. Chem. Phys. 138 094312
[30] Feng Y Q, Cheng L J 2015 RSC Adv. 5 62543
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