Complexity factor for a class of compact stars in f(R,T) gravity
We investigate the concept of complexity factor for a class of compact star in the framework of modified f ( R , T ) gravity. We obtain a generic form of hydrostatic equilibrium equation, express the Einstein field equations, mass function and also physical observation for linear form of function f...
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| Veröffentlicht in: | Astrophysics and space science 2019-11, Vol.364 (11), p.1-9, Article 194 |
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| creator | Abbas, G. Ahmed, Riaz |
| description | We investigate the concept of complexity factor for a class of compact star in the framework of modified
f
(
R
,
T
)
gravity. We obtain a generic form of hydrostatic equilibrium equation, express the Einstein field equations, mass function and also physical observation for linear form of function
f
(
R
,
T
)
=
R
+
2
λ
T
, where
λ
is the coupling parameter,
R
is Ricci scalar and
T
is trace of energy momentum tensor. We have analyzed the properties of compact astrophysical objects like energy density and anisotropic pressure are affected by changing the values of coupling parameter
λ
. We obtained numerical outputs of some physical variables for different chosen values of coupling parameter
λ
to observe the effect of
λ
on these quantities and show these in tabular form for different compact stars
4
U
1820
-
30
,
Her
X
-
1
,
SAX
J
1808.4
-
3658
and
VelaX
-
12
with radii 10, 7.7, 7.07 and 9.99 respectively. We determine structure scalars with orthogonal splitting of the Riemann tensor and with the help of these scalars the complexity factor can be determined. Furthermore, we have checked some astrophysical sources for vanishing complexity factor. |
| doi_str_mv | 10.1007/s10509-019-3688-8 |
| format | Article |
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f
(
R
,
T
)
gravity. We obtain a generic form of hydrostatic equilibrium equation, express the Einstein field equations, mass function and also physical observation for linear form of function
f
(
R
,
T
)
=
R
+
2
λ
T
, where
λ
is the coupling parameter,
R
is Ricci scalar and
T
is trace of energy momentum tensor. We have analyzed the properties of compact astrophysical objects like energy density and anisotropic pressure are affected by changing the values of coupling parameter
λ
. We obtained numerical outputs of some physical variables for different chosen values of coupling parameter
λ
to observe the effect of
λ
on these quantities and show these in tabular form for different compact stars
4
U
1820
-
30
,
Her
X
-
1
,
SAX
J
1808.4
-
3658
and
VelaX
-
12
with radii 10, 7.7, 7.07 and 9.99 respectively. We determine structure scalars with orthogonal splitting of the Riemann tensor and with the help of these scalars the complexity factor can be determined. Furthermore, we have checked some astrophysical sources for vanishing complexity factor.</description><identifier>ISSN: 0004-640X</identifier><identifier>EISSN: 1572-946X</identifier><identifier>DOI: 10.1007/s10509-019-3688-8</identifier><language>eng</language><publisher>Dordrecht: Springer Netherlands</publisher><subject>Astrobiology ; Astronomy ; Astrophysics ; Astrophysics and Astroparticles ; Complexity ; Cosmology ; Coupling ; Einstein equations ; Equilibrium equations ; Flux density ; Gravitation ; Observations and Techniques ; Original Article ; Parameters ; Physics ; Physics and Astronomy ; Scalars ; Space Exploration and Astronautics ; Space Sciences (including Extraterrestrial Physics ; Stars ; Tensors</subject><ispartof>Astrophysics and space science, 2019-11, Vol.364 (11), p.1-9, Article 194</ispartof><rights>Springer Nature B.V. 2019</rights><rights>Astrophysics and Space Science is a copyright of Springer, (2019). All Rights Reserved.</rights><lds50>peer_reviewed</lds50><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c316t-71d1a027de3975ccf11e77c81ff6014e5bbd101f1cf48d3cfd93915c131237353</citedby><cites>FETCH-LOGICAL-c316t-71d1a027de3975ccf11e77c81ff6014e5bbd101f1cf48d3cfd93915c131237353</cites><orcidid>0000-0002-4525-566X</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://link.springer.com/content/pdf/10.1007/s10509-019-3688-8$$EPDF$$P50$$Gspringer$$H</linktopdf><linktohtml>$$Uhttps://link.springer.com/10.1007/s10509-019-3688-8$$EHTML$$P50$$Gspringer$$H</linktohtml><link.rule.ids>314,776,780,27901,27902,41464,42533,51294</link.rule.ids></links><search><creatorcontrib>Abbas, G.</creatorcontrib><creatorcontrib>Ahmed, Riaz</creatorcontrib><title>Complexity factor for a class of compact stars in f(R,T) gravity</title><title>Astrophysics and space science</title><addtitle>Astrophys Space Sci</addtitle><description>We investigate the concept of complexity factor for a class of compact star in the framework of modified
f
(
R
,
T
)
gravity. We obtain a generic form of hydrostatic equilibrium equation, express the Einstein field equations, mass function and also physical observation for linear form of function
f
(
R
,
T
)
=
R
+
2
λ
T
, where
λ
is the coupling parameter,
R
is Ricci scalar and
T
is trace of energy momentum tensor. We have analyzed the properties of compact astrophysical objects like energy density and anisotropic pressure are affected by changing the values of coupling parameter
λ
. We obtained numerical outputs of some physical variables for different chosen values of coupling parameter
λ
to observe the effect of
λ
on these quantities and show these in tabular form for different compact stars
4
U
1820
-
30
,
Her
X
-
1
,
SAX
J
1808.4
-
3658
and
VelaX
-
12
with radii 10, 7.7, 7.07 and 9.99 respectively. We determine structure scalars with orthogonal splitting of the Riemann tensor and with the help of these scalars the complexity factor can be determined. Furthermore, we have checked some astrophysical sources for vanishing complexity factor.</description><subject>Astrobiology</subject><subject>Astronomy</subject><subject>Astrophysics</subject><subject>Astrophysics and Astroparticles</subject><subject>Complexity</subject><subject>Cosmology</subject><subject>Coupling</subject><subject>Einstein equations</subject><subject>Equilibrium equations</subject><subject>Flux density</subject><subject>Gravitation</subject><subject>Observations and Techniques</subject><subject>Original Article</subject><subject>Parameters</subject><subject>Physics</subject><subject>Physics and Astronomy</subject><subject>Scalars</subject><subject>Space Exploration and Astronautics</subject><subject>Space Sciences (including Extraterrestrial Physics</subject><subject>Stars</subject><subject>Tensors</subject><issn>0004-640X</issn><issn>1572-946X</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2019</creationdate><recordtype>article</recordtype><sourceid>BENPR</sourceid><recordid>eNp1kE1LAzEQhoMoWKs_wFvAi4LRmZ3dZHNTil9QEKRCbyHNJqWl7dZkK_bfG1nBk4dhGOZ5ZuBl7BzhBgHUbUKoQAtALUjWtagP2AArVQhdyukhGwBAKWQJ02N2ktIyj1pqNWB3o3a9XfmvRbfnwbqujTzkstytbEq8DdxlIC946mxMfLHh4fLtenLF59F-ZuuUHQW7Sv7stw_Z--PDZPQsxq9PL6P7sXCEshMKG7RQqMaTVpVzAdEr5WoMQQKWvprNGgQM6EJZN-RCo0lj5ZCwIEUVDdlFf3cb24-dT51Ztru4yS9NQUhAVIDMFPaUi21K0QezjYu1jXuDYH6CMn1QJgdlfoIydXaK3kmZ3cx9_Lv8v_QN3yVpZg</recordid><startdate>20191101</startdate><enddate>20191101</enddate><creator>Abbas, G.</creator><creator>Ahmed, Riaz</creator><general>Springer Netherlands</general><general>Springer Nature B.V</general><scope>AAYXX</scope><scope>CITATION</scope><scope>3V.</scope><scope>7TG</scope><scope>7XB</scope><scope>88I</scope><scope>8FD</scope><scope>8FE</scope><scope>8FG</scope><scope>8FK</scope><scope>ABUWG</scope><scope>AEUYN</scope><scope>AFKRA</scope><scope>ARAPS</scope><scope>AZQEC</scope><scope>BENPR</scope><scope>BGLVJ</scope><scope>CCPQU</scope><scope>DWQXO</scope><scope>GNUQQ</scope><scope>H8D</scope><scope>HCIFZ</scope><scope>KL.</scope><scope>L7M</scope><scope>M2P</scope><scope>P5Z</scope><scope>P62</scope><scope>PQEST</scope><scope>PQQKQ</scope><scope>PQUKI</scope><scope>Q9U</scope><orcidid>https://orcid.org/0000-0002-4525-566X</orcidid></search><sort><creationdate>20191101</creationdate><title>Complexity factor for a class of compact stars in f(R,T) gravity</title><author>Abbas, G. ; Ahmed, Riaz</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c316t-71d1a027de3975ccf11e77c81ff6014e5bbd101f1cf48d3cfd93915c131237353</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2019</creationdate><topic>Astrobiology</topic><topic>Astronomy</topic><topic>Astrophysics</topic><topic>Astrophysics and Astroparticles</topic><topic>Complexity</topic><topic>Cosmology</topic><topic>Coupling</topic><topic>Einstein equations</topic><topic>Equilibrium equations</topic><topic>Flux density</topic><topic>Gravitation</topic><topic>Observations and Techniques</topic><topic>Original Article</topic><topic>Parameters</topic><topic>Physics</topic><topic>Physics and Astronomy</topic><topic>Scalars</topic><topic>Space Exploration and Astronautics</topic><topic>Space Sciences (including Extraterrestrial Physics</topic><topic>Stars</topic><topic>Tensors</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Abbas, G.</creatorcontrib><creatorcontrib>Ahmed, Riaz</creatorcontrib><collection>CrossRef</collection><collection>ProQuest Central (Corporate)</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>ProQuest Central (purchase pre-March 2016)</collection><collection>Science Database (Alumni Edition)</collection><collection>Technology Research Database</collection><collection>ProQuest SciTech Collection</collection><collection>ProQuest Technology Collection</collection><collection>ProQuest Central (Alumni) (purchase pre-March 2016)</collection><collection>ProQuest Central (Alumni)</collection><collection>ProQuest One Sustainability</collection><collection>ProQuest Central</collection><collection>Advanced Technologies & Aerospace Database (1962 - current)</collection><collection>ProQuest Central Essentials</collection><collection>ProQuest Central</collection><collection>Technology Collection</collection><collection>ProQuest One Community College</collection><collection>ProQuest Central</collection><collection>ProQuest Central Student</collection><collection>Aerospace Database</collection><collection>SciTech Premium Collection</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>ProQuest Science Journals</collection><collection>ProQuest advanced technologies & aerospace journals</collection><collection>ProQuest Advanced Technologies & Aerospace Collection</collection><collection>ProQuest One Academic Eastern Edition (DO NOT USE)</collection><collection>ProQuest One Academic</collection><collection>ProQuest One Academic UKI Edition</collection><collection>ProQuest Central Basic</collection><jtitle>Astrophysics and space science</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Abbas, G.</au><au>Ahmed, Riaz</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Complexity factor for a class of compact stars in f(R,T) gravity</atitle><jtitle>Astrophysics and space science</jtitle><stitle>Astrophys Space Sci</stitle><date>2019-11-01</date><risdate>2019</risdate><volume>364</volume><issue>11</issue><spage>1</spage><epage>9</epage><pages>1-9</pages><artnum>194</artnum><issn>0004-640X</issn><eissn>1572-946X</eissn><abstract>We investigate the concept of complexity factor for a class of compact star in the framework of modified
f
(
R
,
T
)
gravity. We obtain a generic form of hydrostatic equilibrium equation, express the Einstein field equations, mass function and also physical observation for linear form of function
f
(
R
,
T
)
=
R
+
2
λ
T
, where
λ
is the coupling parameter,
R
is Ricci scalar and
T
is trace of energy momentum tensor. We have analyzed the properties of compact astrophysical objects like energy density and anisotropic pressure are affected by changing the values of coupling parameter
λ
. We obtained numerical outputs of some physical variables for different chosen values of coupling parameter
λ
to observe the effect of
λ
on these quantities and show these in tabular form for different compact stars
4
U
1820
-
30
,
Her
X
-
1
,
SAX
J
1808.4
-
3658
and
VelaX
-
12
with radii 10, 7.7, 7.07 and 9.99 respectively. We determine structure scalars with orthogonal splitting of the Riemann tensor and with the help of these scalars the complexity factor can be determined. Furthermore, we have checked some astrophysical sources for vanishing complexity factor.</abstract><cop>Dordrecht</cop><pub>Springer Netherlands</pub><doi>10.1007/s10509-019-3688-8</doi><tpages>9</tpages><orcidid>https://orcid.org/0000-0002-4525-566X</orcidid></addata></record> |
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| source | SpringerLink (Online service) |
| subjects | Astrobiology Astronomy Astrophysics Astrophysics and Astroparticles Complexity Cosmology Coupling Einstein equations Equilibrium equations Flux density Gravitation Observations and Techniques Original Article Parameters Physics Physics and Astronomy Scalars Space Exploration and Astronautics Space Sciences (including Extraterrestrial Physics Stars Tensors |
| title | Complexity factor for a class of compact stars in f(R,T) gravity |
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