The thermodynamic characteristics of hot and rotating superheavy nucleus <InlineEquation ID="IEq3"> <EquationSource Format="TEX">$Z=120$</EquationSource> <EquationSource Format="MATHML"><math> <mrow> <mi>Z</mi> <mo>=</mo> <mn>120</mn> </mrow> </math></EquationSource> </InlineEquation>, studied through statistical model calculations, reveal a quasi-magic and magic neutron number at <InlineEquation ID="IEq4"> <EquationSource Format="TEX">$N=178$</EquationSource> <EquationSource Format="MATHML"><math> <mrow> <mi>N</mi> <mo>=</mo> <mn>178</mn> </mrow> </math></EquationSource> </InlineEquation> and <InlineEquation ID="IEq5"> <EquationSource Format="TEX">$N=184$</EquationSource> <EquationSource Format="MATHML"><math> <mrow> <mi>N</mi> <mo>=</mo> <mn>184</mn> </mrow> </math></EquationSource> </InlineEquation>, respectively, by considering the thermodynamic temperature at the shape transition from spherical to oblate. The interplay between thermodynamic temperature and neutron separation energy at different temperatures determine the most probable isotope as <InlineEquation ID="IEq6"> <EquationSource Format="TEX">$^{304}$</EquationSource> <EquationSource Format="MATHML"><math> <mmultiscripts> <mrow /> <mrow /> <mn>304</mn> </mmultiscripts> </math></EquationSource> </InlineEquation>120, which is in coincidence with the prediction of relatively high stability at <InlineEquation ID="IEq7"> <EquationSource Format="TEX">$N{\,=\,}184$</EquationSource> <EquationSource Format="MATHML"><math> <mrow> <mi>N</mi> <mrow> <mspace width="0.166667em" /> <mo>=</mo> <mspace width="0.166667em" /> </mrow> <mn>184</mn> </mrow> </math></EquationSource> </InlineEquation> by Oganessian and Utyonkov (Nucl. Phys. A 62, 944 (2015)), self consistent microscopic calculations of Sobiczewski and Pomorski (Prog. Part. Nucl. Phys. 58, 292 (2007)) and RMF calculations by Bhuyan and Patra (Mod. Phys. Lett. A 27, 1250173 (2012)). A novel approach of analyzing the change in thermodynamic temperature delineates the thermodynamic influence on the rotating system, which gives the instability temperature, <InlineEquation ID="IEq8"> <EquationSource Format="TEX">$T_{\lim }\>3.0$</EquationSource> <EquationSource Format="MATHML"><math> <mrow> <msub> <mi>T</mi> <mo movablelimits="true">lim</mo> </msub> <mspace width="0.222222em" /> <mn>3.0</mn> </mrow> </math></EquationSource> </InlineEquation> MeV. Also discussed the feasible temperature for the formation of these isotopes.

Role of thermodynamic temperature in predicting the most feasible isotopes of $Z=120$ and their limiting temperature

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2026年5月13日

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M. Geetha,
S. Santhosh Kumar,
G. Suresh

摘要

The thermodynamic characteristics of hot and rotating superheavy nucleus $Z=120$ $Z = 120$ , studied through statistical model calculations, reveal a quasi-magic and magic neutron number at $N=178$ $N = 178$ and $N=184$ $N = 184$ , respectively, by considering the thermodynamic temperature at the shape transition from spherical to oblate. The interplay between thermodynamic temperature and neutron separation energy at different temperatures determine the most probable isotope as $^{304}$ $^{304}$ 120, which is in coincidence with the prediction of relatively high stability at $N{\,=\,}184$ $N = 184$ by Oganessian and Utyonkov (Nucl. Phys. A 62, 944 (2015)), self consistent microscopic calculations of Sobiczewski and Pomorski (Prog. Part. Nucl. Phys. 58, 292 (2007)) and RMF calculations by Bhuyan and Patra (Mod. Phys. Lett. A 27, 1250173 (2012)). A novel approach of analyzing the change in thermodynamic temperature delineates the thermodynamic influence on the rotating system, which gives the instability temperature, $T_{\lim }\>3.0$ $T_{lim} 3.0$ MeV. Also discussed the feasible temperature for the formation of these isotopes.

Role of thermodynamic temperature in predicting the most feasible isotopes of \(Z=120\) and their limiting temperature

摘要