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From Microscopic to Macroscopic: The Effect of Relativistic Mean Field Parameter Sets on Neutron Star Structure

Jurnal Fisika · Vol. 16 No. 2 (2026) · pp. 128–140

DOI
10.15294/jf.v16i2.47273
ISSN
2684-978X, 2088-1509
Published
2026-10-11
Publisher
Universitas Negeri Semarang
Language
eng

Abstract

Neutron stars, as extremely compact astrophysical objects, provide a unique natural laboratory for investigating the physics of compact matter. Neutron stars can be described from two complementary perspectives, namely microscopic and macroscopic states. The microscopic state is characterized through the relativistic mean-field (RMF) equation of state, which describes the dynamics of dense matter inside the star. The macroscopic state, on the other hand, is described by the Tolman–Oppenheimer–Volkoff (TOV) equations, which determine the global stellar structure. This study aims to examine how the microscopic properties of neutron stars influence their macroscopic behavior by varying the microscopic coupling constants encoded in different RMF parameter sets. The parameter sets employed in this work are taken from well-established and widely validated RMF models in the literature, including NL3, FSUGold, S271, and Z271. Through numerical modeling, the effects of variations in these parameter sets on the maximum mass, radius, energy density, and pressure of neutron stars are systematically investigated. The results demonstrate that the choice of parameter set has a significant impact on the maximum mass that a neutron star can support. In particular, stiffer parameter sets lead to larger maximum masses, whereas softer parameter sets result in smaller maximum masses.

Keywords

Collaboration network of the authors

40 authors · 208 co-authorship links · 2 across different organisations · showing the 40 most connected

Hover or tap a name to highlight its co-authors. Double-click to open the author's page.

  • Universitas Halu Oleo
  • Universitas Muslim Indonesia
  • Universitas Jambi
  • University of Brawijaya
  • Affiliation unknown
  • Different organisations
  • Same organisation
  • Affiliation unknown
  • Thicker line = more joint articles · bigger circle = more articles
Show as table
Co-authorOrganisationJoint articles
Mardian PeslinofAffiliation unknown19
Frastica DeswardaniAffiliation unknown14
Nurhidayah NurhidayahUniversitas Halu Oleo10
Samsidar SamsidarUniversitas Muslim Indonesia10
Linda HandayaniAffiliation unknown9
Tika RestianingsihAffiliation unknown7
Rustan RustanAffiliation unknown6
Iful AmriAffiliation unknown5
Maison MaisonAffiliation unknown5
Benedika Ferdian HutabaratUniversitas Jambi4
Rista Mutia AnggrainiAffiliation unknown4
Cindy Nur SyaqilaAffiliation unknown4
Ilham Jaya WindhanuAffiliation unknown4
NurhidayahAffiliation unknown3
. SamsidarAffiliation unknown3
RustanAffiliation unknown3
Ardiyaningsih Puji LestariAffiliation unknown3
Nova SusantiAffiliation unknown2
NazarudinAffiliation unknown2
NelsonAffiliation unknown2
Sherli YurinandaAffiliation unknown2
Faizar FaridAffiliation unknown2
Rabiah Al AdawiyahAffiliation unknown1
Febri Berthalita PujaningsihAffiliation unknown1
Athanasius CiptaAffiliation unknown1
Samsidah SamsidahAffiliation unknown1
Aulia SanovaAffiliation unknown1
Siti SyuhadaAffiliation unknown1
Muswita MuswitaAffiliation unknown1
Tiara SandariAffiliation unknown1
Helga Dwi FahyuanAffiliation unknown1
Helga DwiAffiliation unknown1
Heriyanti HeriyantiAffiliation unknown1
Sutrisno SutrisnoUniversity of Brawijaya1
Desi AyundariAffiliation unknown1

Affiliations come from OpenAlex; journal OAI-PMH metadata carries none. Authors without an OpenAlex ID are matched by name, which can merge or split people.

Metadata source: OAI-PMH (metadata jurnal) https://journal.unnes.ac.id/journals/jf/oai, first harvested 6 Nov 2026, last seen 6 Nov 2026.
Original metadata (oai_dc) 
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	<dc:title xml:lang="en">From Microscopic to Macroscopic: The Effect of Relativistic Mean Field Parameter Sets on Neutron Star Structure</dc:title>
	<dc:creator xml:lang="en">Alrizal, Alrizal</dc:creator>
	<dc:creator xml:lang="en">Fendriani, Yoza</dc:creator>
	<dc:creator xml:lang="en">Afrianto, M. Ficky </dc:creator>
	<dc:creator xml:lang="en">Pebralia, Jesi</dc:creator>
	<dc:creator xml:lang="en">Tane, Fairuz Athaya zahran Tane</dc:creator>
	<dc:subject xml:lang="en">Neutron Star</dc:subject>
	<dc:subject xml:lang="en">Equation of State</dc:subject>
	<dc:subject xml:lang="en"> Relativistic Mean Field.</dc:subject>
	<dc:description xml:lang="en">Neutron stars, as extremely compact astrophysical objects, provide a unique natural laboratory for investigating the physics of compact matter. Neutron stars can be described from two complementary perspectives, namely microscopic and macroscopic states. The microscopic state is characterized through the relativistic mean-field (RMF) equation of state, which describes the dynamics of dense matter inside the star. The macroscopic state, on the other hand, is described by the Tolman–Oppenheimer–Volkoff (TOV) equations, which determine the global stellar structure. This study aims to examine how the microscopic properties of neutron stars influence their macroscopic behavior by varying the microscopic coupling constants encoded in different RMF parameter sets. The parameter sets employed in this work are taken from well-established and widely validated RMF models in the literature, including NL3, FSUGold, S271, and Z271. Through numerical modeling, the effects of variations in these parameter sets on the maximum mass, radius, energy density, and pressure of neutron stars are systematically investigated. The results demonstrate that the choice of parameter set has a significant impact on the maximum mass that a neutron star can support. In particular, stiffer parameter sets lead to larger maximum masses, whereas softer parameter sets result in smaller maximum masses.</dc:description>
	<dc:publisher xml:lang="en">Universitas Negeri Semarang</dc:publisher>
	<dc:date>2026-10-11</dc:date>
	<dc:type>info:eu-repo/semantics/article</dc:type>
	<dc:type>info:eu-repo/semantics/publishedVersion</dc:type>
	<dc:type xml:lang="en">Peer-reviewed Article</dc:type>
	<dc:format>application/pdf</dc:format>
	<dc:identifier>https://journal.unnes.ac.id/journals/jf/article/view/47273</dc:identifier>
	<dc:identifier>10.15294/jf.v16i2.47273</dc:identifier>
	<dc:source xml:lang="en">Jurnal Fisika; Vol. 16 No. 2 (2026): Jurnal Fisika 16 (2) 2026; 128-140</dc:source>
	<dc:source>2684-978X</dc:source>
	<dc:source>2088-1509</dc:source>
	<dc:source>10.15294/jf.v16i2</dc:source>
	<dc:language>eng</dc:language>
	<dc:relation>https://journal.unnes.ac.id/journals/jf/article/view/47273/11690</dc:relation>
	<dc:rights xml:lang="en">Copyright (c) 2026 Jurnal Fisika</dc:rights>
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