We investigate the possibility to explain theoretically the S2 star orbital precession around the massive object at Galactic Centre using Extended Theories of Gravity, specifically f(R, φ) a Sanders-like gravitational potential in total absence of dark matter. To this aim an analytic fourth-order theory of gravity, non-minimally coupled with a massive scalar field is considered. The interaction term is given by an analytic functions f(R, φ) where R is the Ricci scalar and φ is the scalar field. We simulated orbit of S2 star around Galactic Centre in Sanders-like gravity potentials and compared it with NTT/VLT observations. We presented maps of reduced χ 2 over the {α − mφ} parameter space in the case of NTT/VLT observations. The approach we are proposing seems reliable to constrain modified gravity models at astronomical level

Borka Jovanović, Vesna

Borka, Duško

Capozziello, Salvatore

Jovanović, Predrag

English

Repository of the Vinča Nuclear Institute (VinaR)

Publ. Astron. Obs. Belgrade No. 96 (2017), 205 - 210 Contributed PaperCONSTRAINTS ON f(R, φ) (SANDERS-LIKE)GRAVITY POTENTIAL FROM ORBIT OF S2 STARD. BORKA1, P. JOVANOVIĆ2, V. BORKA JOVANOVIĆ1 and S. CAPOZZIELLO3,4,51Atomic Physics Laboratory (040), Vinča Institute of Nuclear Sciences,University of Belgrade, P.O. Box 522, 11001 Belgrade, SerbiaE–mail: dusborka@vinca.rsE–mail: vborka@vinca.rs2Astronomical Observatory, Volgina 7, 11060 Belgrade, SerbiaE–mail: pjovanovic@aob.rs3Dipartimento di Fisica, Università di Napoli ”Federico II”, Compl. Univ.di Monte S. Angelo, Edificio G, Via Cinthia, I-80126, Napoli, Italy4INFN Sez. di Napoli, Compl. Univ. di Monte S.Angelo, Edificio G, Via Cinthia, I-80126, Napoli, Italy5Gran Sasso Science Institute (INFN), Viale F. Crispi, 7, I-67100, L’Aquila, ItalyE–mail: capozziello@na.infn.itAbstract. We investigate the possibility to explain theoretically the S2 star orbital pre-cession around the massive object at Galactic Centre using Extended Theories of Gravity,specifically f(R, φ) a Sanders-like gravitational potential in total absence of dark matter. Tothis aim an analytic fourth-order theory of gravity, non-minimally coupled with a massivescalar field is considered. The interaction term is given by an analytic functions f(R, φ)where R is the Ricci scalar and φ is the scalar field. We simulated orbit of S2 star aroundGalactic Centre in Sanders-like gravity potentials and compared it with NTT/VLT obser-vations. We presented maps of reduced χ2 over the {α − mφ} parameter space in thecase of NTT/VLT observations. The approach we are proposing seems reliable to constrainmodified gravity models at astronomical level.1. INTRODUCTIONExtended Theories of Gravity (see e.g. Capozziello & De Laurentis 2011) are alter-native theories of gravitational interaction. These theories are developed from theexact starting points like General Relativity. They aimed from one side to extend thepositive results of General Relativity and, on the other hand, to cure its shortcomings.These theories have been proposed like alternative approaches to Newtonian gravityin order to explain galactic and extragalactic dynamics without introducing dark mat-ter (see e.g. Capozziello & De Laurentis 2012, Nojiri & Odintsov 2011, Capozziello205D. BORKA et al.2002, Capozziello et al. 2003, Capozziello & Faraoni 2010).S-stars closely orbit the massive compact object at the center of Milky Way, namedSgr A∗ (see e.g. Ghez et al. 2000, Gillessen et al. 2009a, Gillessen et al. 2009b, Genzelet al. 2010). These stars, together with recently discovered dense gas cloud fallingtowards the Galactic Centre (see e.g. Gillessen et al. 2012), indicate that the massivecentral object is probably a black hole. There are some observational indications, forat least S2, that its orbit may deviate from the Keplerian case (see e.g. Gillessen etal. 2009a, Meyer et al. 2012).2. THEORY2. 1. f(R, φ) THEORIES OF GRAVITYWe can consider a generic function of Ricci scalar and scalar field. Then the actionbecomes (see e.g. Stabile & Capozziello 2013):A =∫d4x√−g[f(R,φ) + ω(φ)φ;α φ;α + XLm]. (1)We get φ = φ(0) + φ(1) + φ(2) + . . . and the function f(R,φ) with its partialderivatives (fR, fRR, fφ, fφφ and fφR) and ω(φ) can be substituted by their corre-sponding Taylor series. In the case of f(R, φ), we have:f(R,φ) ∼ f(0, φ(0)) + fR(0, φ(0))R(1) + fφ(0, φ(0))φ(1)... (2)In the f(R, φ)-gravity the gravitational potential is found by setting the gravita-tional constant asG =(2 ω(φ(0)) φ(0) − 42 ω(φ(0)) φ(0) − 3)G∞φ(0)(3)where G∞ is the gravitational constant as measured at infinity and by imposingα−1 = 3 − 2 ω(φ(0)) φ(0), the gravity potential is (see e.g. Stabile & Capozziello2013):ΦST (x) = −G∞M|x|{1 + α e−√1−3α mφ|x|}(4)and then a Sanders-like potential is obtained (see e.g. Sanders 1990, Sanders 1984).2. 2. SIMULATED ORBITS OF S2 STARIn order to constrain the parameters of f(R,φ) model, we simulate orbits of S2 star inSanders-like gravity potentials. We fit orbits to the astrometric observations obtainedby New Technology Telescope/Very Large Telescope (NTT/VLT) (see e.g. Gilessenet al. 2009a) for different combinations of α and mφ. Each simulated orbit is definedby four initial conditions: two components of initial position and two componentsof initial velocity in orbital plane at the epoch of the first observation. For eachcombination of α and mφ, we obtain the best fit initial conditions corresponding toa simulated orbit. The fitting procedure is performed using LMDIF1 routine fromMINPACK-1 Fortran 77 library which solves the nonlinear least squares problemsby a modification of Marquardt-Levenberg algorithm (see e.g. Moré et al. 1980).Detailed descriptions are given in the papers of Borka et al. (2012, 2013).206CONSTRAINTS ON f(R, φ) (SANDERS-LIKE) GRAVITY POTENTIAL FROM ORBIT OF S2 STAR 1.801.701.601.551.520.00 0.05 0.10 0.15 0.20 0.25 0.30α0.000.010.020.030.040.050.06mΦ1.551.601.651.701.751.801.85χ2Figure 1: The map of reduced χ2 over the {α−mφ} parameter space of f(R, φ) gravityin case of NTT/VLT observations of S2 star which give at least the same (χ2 = 1.89)or better fits (χ2 < 1.89) than the Keplerian orbits. The map corresponds to mφ in[0, 0.06] and α in [0, 0.33]. A few contours are presented for specific values of reducedχ2 given in the legend. 1.801.701.601.551.511.500.0001 0.0002 0.0003 0.0004 0.0005 0.0006α-0.0030-0.0028-0.0026-0.0024-0.0022-0.0020mΦ1.551.601.651.701.751.801.85χ2Figure 2: The same as in Figure 1, but for a narrow region in the {α−mφ} parameterspace around the absolute minimum of the reduced χ2. A few contours are presentedfor specific values of reduced χ2 given in the legend.207D. BORKA et al.-0.0004 -0.0002 0.0000 0.0002 0.0004-0.0030-0.0029-0.0028-0.0027-0.0026-0.0025ΑmΦDΘH°L-20-1001020Figure 3: Numerically calculated angle of precession per orbital period as function ofparameters α in the range [−0.0005, 0.0005] and mφ in the range [−0.003,−0.0025]in case of Sanders-like potential. The pericenter advance (like in GR) is obtained forpositive α, and retrograde precession for negative α.Figure 4: Comparison between the orbit of S2 star in Newtonian potential (red dashedline) and Sanders-like potential for the best fit parameters α = 0.00018 and mφ =-0.0026 during 5 orbital periods (blue solid line).208CONSTRAINTS ON f(R, φ) (SANDERS-LIKE) GRAVITY POTENTIAL FROM ORBIT OF S2 STARFigure 5: The same as in Figure 4, but for 15 orbital periods.3. f(R, φ) RESULTS AND DISCUSSIONOur aim in this paper is to determine coefficients f0, fR, fRR, fφ, fφφ and fφR.For more details (see e.g. Stabile & Capozziello 2013, Capozziello et al. 2014). Weobtained the following set of parameters f0 = 0, fR = 3 − 1/α, fφ = 0, fRR = 0,fφR = 1 and fφφ = −m2φ. These choices are physically reliable and mean that we canassume an asymptotic Minkowski background, i.e. f0 = 0, that the General Relativityis recovered for fφ = 0, fRR = 0, fφR = 1, and effective massive modes (and theneffective lengths) are related to fR = 3− 1/α, and fφφ = −m2φ. In particular, f0 = 0means that cosmological constant can be discarded at local scales.Figures 1 and 2 presented the maps of the reduced χ2 over the {α−mφ} parameterspace in f(R,φ) gravity for all simulated orbits of S2 star which give at least the sameor better fits than the Keplerian orbits (χ2 = 1.89). Figure 1 corresponds to mφ in[0, 0.06] and α in [0, 0.33]. Figure 2 corresponds to the zoomed range of parametersmφ and α. For α < 0, there is no region in the parameter space where χ2 < 1.89(Keplerian case). For 0 < α < 1/3 there are two regions where χ2 < 1.89 (for mφ < 0and mφ > 0), but the absolute minimum is for mφ < 0. We obtained absoluteminimum of the reduced χ2 for α in the interval [0.0001, 0.0004], and mφ in theinterval [−0.0029,−0.0023]. The absolute minimum of the reduced χ2 (χ2 = 1.5011)is obtained for α = 0.00018 and mφ = -0.0026, respectively.Graphical presentation of precession per orbital period for α in the range [−0.0005,0.0005] and mφ in [−0.003,−0.0025] is given in Figure 3. As one can see pericenteradvance (like in GR) is obtained for positive α, and retrograde precession for negativeα. The fits better than Keplerian are obtained only for positive α, i.e. for theprecession in the same direction as in GR.209D. BORKA et al.The simulated orbits of S2 star around the Galactic Centre in Sanders gravitypotential (blue solid line) and in Newtonian gravity potential (red dashed line) forα = 0.00018 and mφ = -0.0026 during 5 and 15 periods, are presented in Figure 4and Figure 5, respectively. We can see from Figures 4 and 5 that the best fit orbitin Sanders gravity potential precesses for about 3◦.1 per orbital period. GeneralRelativity predicts that pericenter of S2 star should advance by 0◦.08 per orbitalrevolution (see e.g. Gillessen et al. 2009b) which is much smaller than the value ofprecession per orbital period in Sanders gravity potential, but the direction of theprecession is the same.AcknowledgmentsD.B., P.J. and V.B.J. wish to acknowledge the support by the Ministry of Education,Science and Technological Development of the Republic of Serbia through the project176003. S.C. acknowledges the support of INFN (iniziativa specifica TEONGRAV).ReferencesBorka, D., Jovanović, P., Borka Jovanović, V., Zakharov, A. F.: 2012, Phys. Rev. D, 85,124004.Borka, D., Jovanović, P., Borka Jovanović, V., Zakharov, A. F.: 2013, JCAP, 11, 050.Capozziello, S., Borka, D. Jovanović, P., Borka Jovanović, V.: 2014, Phys. Rev. D, 90,044052.Capozziello, S.: 2002, Int. J. Mod. Phys. D, 11, 483.Capozziello, S., Cardone, V.F., Carloni, S., Troisi, A.: 2003, Int. J. Mod. Phys. D, 12,1969.Capozziello, S. & Faraoni, V.: Beyond Einstein gravity: A Survey of gravitational theoriesfor cosmology and astrophysics, Fundamental Theories of Physics, Vol. 170, Springer,New York (2010).Capozziello, S. & De Laurentis, M.: 2011, Physics Reports, 509, 167.Capozziello, S. & De Laurentis, M.: 2012, Ann. Phys., 524, 545.Genzel, R. et al.: 2010, Rev. Mod. Phys., 82, 3121.Ghez, A. M. et al.: 2000, Nature, 407, 349.Gillessen, S. et al.: 2009a, Astrophys. J., 707, L114.Gillessen S. et al.: 2009b, Astrophys. J., 692, 1075.Gillessen, S. et al.: 2012, Nature, 481, 51.Meyer, L. et al.: 2012, Science, 338, 84.Moré, J. J., Garbow, B. S., Hillstrom, K. E.: 1980, User Guide for MINPACK-1, ArgonneNational Laboratory Report ANL-80-74, Argonne, Ill.Nojiri, S. & Odintsov, S. D.: 2011, Physics Reports, 505, 59.Sanders, R. H.: 1990, Ann. Rev. Astron. Astrophys., 2, 1.Sanders, R. H.: 1984, Astron. Astrophys., 136, L21.Stabile, A. & Capozziello, S.: 2013, Phys. Rev. D, 87, 064002.210

Constraints on f(R, ɸ) (Sanders-Like) Gravity Potential From Orbit of S2 Star

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Constraints on f(R, ɸ) (Sanders-Like) Gravity Potential From Orbit of S2 Star

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