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Uma Papnoi

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Katherine Butler Schofield

King's College London

Prof. Dr. Raffaele Pisano, MSc, HDR (Habil.)

Université des Sciences et Technologies de Lille (Lille-1)

University of Hyderabad

Javier Marín-López

Universidad de Jaén

Universidade Estadual Paulista "Júlio de Mesquita Filho"

Luigi Collarile

Bern University of Applied Sciences

Nikos Mantzakouras

National & Kapodistrian University of Athens

Thomas Curtright

University of Miami

University of East London

Gwen Robbins Schug

University of North Carolina at Greensboro

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Papers by Uma Papnoi

185 悪性腫瘍肝転移における 5'-Nucleotide phosphodiesterase-V の腫瘍 marker としての意義 : 他の腫瘍 marker との比較検討( 第23回日本消化器外科学会総会)

25 Push 式小腸ファイバースコープにより術前に確定診断された原発性空腸癌の一例( 第20回日本消化器外科学会総会)

343 回腸・結腸クローン病の1例( 第16回日本消化器外科学会総会)

198 治療に困難を来たした小腸広範囲切除の一例( 第15回日本消化器外科学会総会)

297 新生児期・乳児期に発症した膵島細胞症4例の術後遠隔成績

Rotating charged black hole in 4D Einstein–Gauss–Bonnet gravity: Photon motion and its shadow

Physics of the Dark Universe, 2022

Resumo: A pandemia do novo coronavírus (SARS-CoV-2) contaminou mais de 22 milhões de pessoas na T... more Resumo: A pandemia do novo coronavírus (SARS-CoV-2) contaminou mais de 22 milhões de pessoas na Terra e estima-se que, em 2021, mais de seis centenas de milhares de cidadãos venham a óbito no Brasil. A convivência com as variantes do vírus deverá ocorrer, pelo menos, até 2022, cabendo aos três níveis de governo agirem em conjunto no seu enfrentamento. O "Novo Normal "exige um ambiente renovado e demanda a adoção da sustentabilidade socioambiental nas unidades escolares do ensino básico brasileiro. O modelo do Programa Nacional de Escolas Sustentáveis associado ao Programa Dinheiro Direto na Escola e a Agenda Ambiental Federal devem ser devidamente ressignificados e operacionalizados como políticas públicas integradas e transversais no país.

Optical and Thermodynamic Properties of a Rotating Dyonic Black Hole Spacetime in 𝒩 = 2, U(1)^2 gauged supergravity

The null geodesics and the distance of closest approach for photon around a rotating dyonic black... more The null geodesics and the distance of closest approach for photon around a rotating dyonic black hole in 𝒩 = 2, U(1)^2 gauged supergravity is studied. The phenomenon of black hole shadows with various black hole parameters has also analyzed. Further, the investigation of various thermodynamic properties for this black hole is performed with various thermodynamic parameters at the horizon. The heat capacity to study the thermodynamic stability of this black hole spacetime is also studied. The influence for different values of the black hole parameters ν, e, ν, g and N_g on the phenomenon of black hole shadows and thermodynamic parameters is also investigated visually.

Thermodynamic structure of field equations near apparent horizon for radiating black holes

We study the intriguing analogy between gravitational dynamics of the horizon and thermodynamics ... more We study the intriguing analogy between gravitational dynamics of the horizon and thermodynamics for the case of nonstationary radiating spherically symmetric black holes both in four dimensions and higher dimensions. By defining all kinematical parameters of nonstationary radiating black holes in terms of null vectors, we demonstrate that it is possible to interpret the Einstein field equations near the apparent horizon in the form of a thermodynamical identity TdS=dE+PdV.

Spinning Higher Dimensional Einstein-Yang-Mills black holes

We construct a Kerr-Newman-like spacetimes starting from higher dimensional (HD) Einstein-Yang-Mi... more We construct a Kerr-Newman-like spacetimes starting from higher dimensional (HD) Einstein-Yang-Mills black holes via complex transformations suggested by Newman-Janis. The new metrics are HD generalization of Kerr-Newman spacetimes which has a geometry precisely that of Kerr-Newman in 4D corresponding to Yang-Mills (YM) gauge charge, but the sign of charge term gets flipped in the HD spacetimes. It is interesting to note that gravitational contribution of YM gauge charge, in HD, is indeed opposite (attractive rather than repulsive) that of Maxwell charge. The effect of YM gauge charge on the structure and location of static limit surface and apparent horizon is discussed. We find that static limit surfaces become less prolate with increase in dimensions and are also sensitive to YM gauge charge thereby affecting the shape of ergosphere. We also analyze some thermodynamical properties of these BHs.

Clouds of strings in third-order Lovelock gravity

Lovelock theory is a natural extension of the Einstein theory of general relativity to higher dim... more Lovelock theory is a natural extension of the Einstein theory of general relativity to higher dimensions in which the first and second orders correspond, respectively, to general relativity and Einstein-Gauss-Bonnet gravity. We present exact black hole solutions of D≥ 4-dimensional spacetime for first-, second-, and third-order Lovelock gravities in a string cloud background. Further, we compute the mass, temperature, and entropy of black hole solutions for the higher-dimensional general relativity and Einstein-Gauss-Bonnet theories and also perform thermodynamic stability of black holes. It turns out that the presence of the Gauss-Bonnet term and/or background string cloud completely changes the black hole thermodynamics. Interestingly, the entropy of a black hole is unaffected due to a background string cloud. We rediscover several known spherically symmetric black hole solutions in the appropriate limits.

14.小型円形陰影を呈した細気管支肺胞上皮癌(GOBLET Cell TYPE)の一例:71回肺癌学会関東支部

肺癌, Dec 25, 1981

Shadow of five-dimensional rotating Myers-Perry black hole

Physical Review D, 2014

A black hole casts a shadow as an optical appearance because of its strong gravitational field. W... more A black hole casts a shadow as an optical appearance because of its strong gravitational field. We study the shadow cast by the five-dimensional Myers-Perry black hole with equal rotation parameters. We demonstrate that the null geodesic equations can be integrated that allows us to investigate the shadow cast by a black hole. The shadow of a black hole is found to be a dark zone covered by deformed circle. Interestingly, the shapes of the black hole shadow are more distorted and size decreases for larger black hole spins. Interestingly, it turns out that, for fixed values of rotation parameter, the shadow is slightly smaller and less deformed than for its four-dimensional Kerr black counterpart. Further, the shadow of the five-dimensional Kerr black hole is concentric deformed circles. The effect of rotation parameter on the shape and size of a naked singularity shadow is also analyzed.

Radiating Kerr-Newman black hole in f(R) gravity

We derive an exact radiating Kerr-Newman like black hole solution, with constant curvature R=R_0 ... more We derive an exact radiating Kerr-Newman like black hole solution, with constant curvature R=R_0 imposed, to metric f(R) gravity via complex transformations suggested by Newman-Janis. This generates a geometry which is precisely that of radiating Kerr-Newman-de Sitter / anti-de Sitter with the f(R) gravity contributing an R_0 cosmological-like term. The structure of three horizon-like surfaces, viz. timelike limit surface, apparent horizon and event horizon, are determined. We demonstrate the existence of an additional cosmological horizon, in f(R) gravity model, apart from the regular black hole horizons that exist in the analogous general relativity case. In particular, the known stationary Kerr-Newman black hole solutions of f(R) gravity and general relativity are retrieved. We find that the timelike limit surface becomes less prolate with R_0 thereby affecting the shape of the corresponding ergosphere.

J un 2 01 3 Radiating Kerr-Newman black hole in f ( R ) gravity

We derive an exact radiating Kerr-Newman like black hole solution, with constant curvature R = R0... more We derive an exact radiating Kerr-Newman like black hole solution, with constant curvature R = R0 imposed, to metric f(R) gravity via complex transformations suggested by Newman-Janis. This generates a geometry which is precisely that of radiating Kerr-Newman-de Sitter / anti-de Sitter with the f(R) gravity contributing an R0 cosmological-like term. The structure of three horizonlike surfaces, viz. timelike limit surface, apparent horizon and event horizon, are determined. We demonstrate the existence of an additional cosmological horizon, in f(R) gravity model, apart from the regular black hole horizons that exist in the analogous general relativity case. In particular, the known stationary Kerr-Newman black hole solutions of f(R) gravity and general relativity are retrieved. We find that the timelike limit surface becomes less prolate with R0 thereby affecting the shape of the corresponding ergosphere.

Shadow of charged rotating black hole surrounded by perfect fluid dark matter

Farruh Atamurotov 2, 3, ∗ and Uma Papnoi 5, † Inha University in Tashkent, Ziyolilar 9, Tashkent ... more Farruh Atamurotov 2, 3, ∗ and Uma Papnoi 5, † Inha University in Tashkent, Ziyolilar 9, Tashkent 100170, Uzbekistan Akfa University, Kichik Halqa Yuli Street 17, Tashkent 100095, Uzbekistan Ulugh Beg Astronomical Institute, Astronomy St. 33, Tashkent 100052, Uzbekistan Gurukul Kangri (Deemed to be University) Vishwavidyalaya, Haridwar 249404, Uttarakhand, India Kanoria PG Mahila Mahavidyalaya, Jaipur 302004, Rajasthan, India

Shadow and deflection angle of charged rotating black hole surrounded by perfect fluid dark matter

Classical and Quantum Gravity

We analysed the shadow cast by charged rotating black hole (BH) in presence of perfect fluid dark... more We analysed the shadow cast by charged rotating black hole (BH) in presence of perfect fluid dark matter (PFDM). We studied the null geodesic equations and obtained the shadow of the charged rotating BH to see the effects of PFDM parameter $\gamma$, charge $Q$ and rotation parameter $a$, and it is noticed that the size as well as the shape of BH shadow is affected due to PFDM parameter, charge and rotation parameter. Thus, it is seen that the presence of dark matter around a BH affects its spacetime. We also investigated the influence of all the parameters (PFDM parameter $\gamma$, BHs charge $Q$ and rotational parameter $a$) on effective potential, energy emission by graphical representation, and compare all the results with the non rotating case in usual general relativity. To this end, we have also explored the effect of PFDM on the deflection angle and the size of Einstein rings.

$Research paper thumbnail of Optical and thermodynamic properties of a rotating dyonic black hole spacetime in $${\mathcal {N}} = 2, U(1)^2$$ gauged supergravity$

Optical and thermodynamic properties of a rotating dyonic black hole spacetime in $${\mathcal {N}} = 2, U(1)^2$$ gauged supergravity

The null geodesics and the distance of closest approach for photon around a rotating dyonic black... more The null geodesics and the distance of closest approach for photon around a rotating dyonic black hole in N = 2, U(1) gauged supergravity is studied. The phenomenon of black hole shadows with various black hole parameters has also analyzed. Further, the investigation of various thermodynamic properties for this black hole is performed with various thermodynamic parameters at the horizon. The heat capacity to study the thermodynamic stability of this black hole spacetime is also studied. The influence for different values of the black hole parameters ν, e, ν, g and Ng on the phenomenon of black hole shadows and thermodynamic parameters is also investigated visually.

Strong gravitational lensing in 5D Myers-Perry black hole spacetime

We study the motion of massless test particles in a five dimensional (5D) Myers-Perry black hole ... more We study the motion of massless test particles in a five dimensional (5D) Myers-Perry black hole spacetime with two spin parameters. The behaviour of the effective potential in view of different values of black hole parameters is discussed in the equatorial plane. The frequency shift of photons is calculated which is found to depend on the spin parameter of black hole and the observed redshift is discussed accordingly. The deflection angle and the strong deflection limit coefficients are also calculated and their behaviour with the spin parameters is analysed in detail. It is observed that the behaviour of both deflection angle and strong field coefficient differs from Kerr black hole spacetime in four dimensions (4D) in General Relativity (GR) mainly due to the presence of two spin parameters in higher dimension.

Thermodynamics from field equations for charged radiating rotating black hole near horizon

International Journal of Modern Physics A

It is well known that near horizon black hole space–times show a resemblance to thermodynamic sys... more It is well known that near horizon black hole space–times show a resemblance to thermodynamic systems, it is easy to associate the thermodynamic parameters like temperature and entropy with them. In this paper, we study the connection between gravitational dynamics of the horizon and thermodynamics for the case of charged radiating rotating axially symmetric black holes. It is shown that Einstein field equation near apparent horizon can be interpreted in the form of thermodynamic law, i.e. [Formula: see text].

Strong lensing and observables around 5D Myers–Perry black hole spacetime

Modern Physics Letters A

We study the motion of massless test particles in a five-dimensional (5D) Myers–Perry black hole ... more We study the motion of massless test particles in a five-dimensional (5D) Myers–Perry black hole spacetime with two-spin parameters. The behavior of the effective potential in view of different values of black hole parameters is discussed in the equatorial plane. The frequency shift of photons is calculated which is found to depend on the spin parameter of black hole and the observed redshift is discussed accordingly. The deflection angle and the strong deflection limit coefficients are also calculated and their behavior with the spin parameters is analyzed in detail. It is observed that the behaviors of both deflection angle and strong field coefficient differs from Kerr black hole spacetime in four dimensions in General Relativity (GR), which is mainly due to the presence of two-spin parameters in higher dimension.

185 悪性腫瘍肝転移における 5'-Nucleotide phosphodiesterase-V の腫瘍 marker としての意義 : 他の腫瘍 marker との比較検討( 第23回日本消化器外科学会総会)

25 Push 式小腸ファイバースコープにより術前に確定診断された原発性空腸癌の一例( 第20回日本消化器外科学会総会)

343 回腸・結腸クローン病の1例( 第16回日本消化器外科学会総会)

198 治療に困難を来たした小腸広範囲切除の一例( 第15回日本消化器外科学会総会)

297 新生児期・乳児期に発症した膵島細胞症4例の術後遠隔成績

Rotating charged black hole in 4D Einstein–Gauss–Bonnet gravity: Photon motion and its shadow

Physics of the Dark Universe, 2022

Resumo: A pandemia do novo coronavírus (SARS-CoV-2) contaminou mais de 22 milhões de pessoas na T... more Resumo: A pandemia do novo coronavírus (SARS-CoV-2) contaminou mais de 22 milhões de pessoas na Terra e estima-se que, em 2021, mais de seis centenas de milhares de cidadãos venham a óbito no Brasil. A convivência com as variantes do vírus deverá ocorrer, pelo menos, até 2022, cabendo aos três níveis de governo agirem em conjunto no seu enfrentamento. O "Novo Normal "exige um ambiente renovado e demanda a adoção da sustentabilidade socioambiental nas unidades escolares do ensino básico brasileiro. O modelo do Programa Nacional de Escolas Sustentáveis associado ao Programa Dinheiro Direto na Escola e a Agenda Ambiental Federal devem ser devidamente ressignificados e operacionalizados como políticas públicas integradas e transversais no país.

Optical and Thermodynamic Properties of a Rotating Dyonic Black Hole Spacetime in 𝒩 = 2, U(1)^2 gauged supergravity

The null geodesics and the distance of closest approach for photon around a rotating dyonic black... more The null geodesics and the distance of closest approach for photon around a rotating dyonic black hole in 𝒩 = 2, U(1)^2 gauged supergravity is studied. The phenomenon of black hole shadows with various black hole parameters has also analyzed. Further, the investigation of various thermodynamic properties for this black hole is performed with various thermodynamic parameters at the horizon. The heat capacity to study the thermodynamic stability of this black hole spacetime is also studied. The influence for different values of the black hole parameters ν, e, ν, g and N_g on the phenomenon of black hole shadows and thermodynamic parameters is also investigated visually.

Thermodynamic structure of field equations near apparent horizon for radiating black holes

We study the intriguing analogy between gravitational dynamics of the horizon and thermodynamics ... more We study the intriguing analogy between gravitational dynamics of the horizon and thermodynamics for the case of nonstationary radiating spherically symmetric black holes both in four dimensions and higher dimensions. By defining all kinematical parameters of nonstationary radiating black holes in terms of null vectors, we demonstrate that it is possible to interpret the Einstein field equations near the apparent horizon in the form of a thermodynamical identity TdS=dE+PdV.

Spinning Higher Dimensional Einstein-Yang-Mills black holes

We construct a Kerr-Newman-like spacetimes starting from higher dimensional (HD) Einstein-Yang-Mi... more We construct a Kerr-Newman-like spacetimes starting from higher dimensional (HD) Einstein-Yang-Mills black holes via complex transformations suggested by Newman-Janis. The new metrics are HD generalization of Kerr-Newman spacetimes which has a geometry precisely that of Kerr-Newman in 4D corresponding to Yang-Mills (YM) gauge charge, but the sign of charge term gets flipped in the HD spacetimes. It is interesting to note that gravitational contribution of YM gauge charge, in HD, is indeed opposite (attractive rather than repulsive) that of Maxwell charge. The effect of YM gauge charge on the structure and location of static limit surface and apparent horizon is discussed. We find that static limit surfaces become less prolate with increase in dimensions and are also sensitive to YM gauge charge thereby affecting the shape of ergosphere. We also analyze some thermodynamical properties of these BHs.

Clouds of strings in third-order Lovelock gravity

Lovelock theory is a natural extension of the Einstein theory of general relativity to higher dim... more Lovelock theory is a natural extension of the Einstein theory of general relativity to higher dimensions in which the first and second orders correspond, respectively, to general relativity and Einstein-Gauss-Bonnet gravity. We present exact black hole solutions of D≥ 4-dimensional spacetime for first-, second-, and third-order Lovelock gravities in a string cloud background. Further, we compute the mass, temperature, and entropy of black hole solutions for the higher-dimensional general relativity and Einstein-Gauss-Bonnet theories and also perform thermodynamic stability of black holes. It turns out that the presence of the Gauss-Bonnet term and/or background string cloud completely changes the black hole thermodynamics. Interestingly, the entropy of a black hole is unaffected due to a background string cloud. We rediscover several known spherically symmetric black hole solutions in the appropriate limits.

14.小型円形陰影を呈した細気管支肺胞上皮癌(GOBLET Cell TYPE)の一例:71回肺癌学会関東支部

肺癌, Dec 25, 1981

Shadow of five-dimensional rotating Myers-Perry black hole

Physical Review D, 2014

A black hole casts a shadow as an optical appearance because of its strong gravitational field. W... more A black hole casts a shadow as an optical appearance because of its strong gravitational field. We study the shadow cast by the five-dimensional Myers-Perry black hole with equal rotation parameters. We demonstrate that the null geodesic equations can be integrated that allows us to investigate the shadow cast by a black hole. The shadow of a black hole is found to be a dark zone covered by deformed circle. Interestingly, the shapes of the black hole shadow are more distorted and size decreases for larger black hole spins. Interestingly, it turns out that, for fixed values of rotation parameter, the shadow is slightly smaller and less deformed than for its four-dimensional Kerr black counterpart. Further, the shadow of the five-dimensional Kerr black hole is concentric deformed circles. The effect of rotation parameter on the shape and size of a naked singularity shadow is also analyzed.

Radiating Kerr-Newman black hole in f(R) gravity

We derive an exact radiating Kerr-Newman like black hole solution, with constant curvature R=R_0 ... more We derive an exact radiating Kerr-Newman like black hole solution, with constant curvature R=R_0 imposed, to metric f(R) gravity via complex transformations suggested by Newman-Janis. This generates a geometry which is precisely that of radiating Kerr-Newman-de Sitter / anti-de Sitter with the f(R) gravity contributing an R_0 cosmological-like term. The structure of three horizon-like surfaces, viz. timelike limit surface, apparent horizon and event horizon, are determined. We demonstrate the existence of an additional cosmological horizon, in f(R) gravity model, apart from the regular black hole horizons that exist in the analogous general relativity case. In particular, the known stationary Kerr-Newman black hole solutions of f(R) gravity and general relativity are retrieved. We find that the timelike limit surface becomes less prolate with R_0 thereby affecting the shape of the corresponding ergosphere.

J un 2 01 3 Radiating Kerr-Newman black hole in f ( R ) gravity

We derive an exact radiating Kerr-Newman like black hole solution, with constant curvature R = R0... more We derive an exact radiating Kerr-Newman like black hole solution, with constant curvature R = R0 imposed, to metric f(R) gravity via complex transformations suggested by Newman-Janis. This generates a geometry which is precisely that of radiating Kerr-Newman-de Sitter / anti-de Sitter with the f(R) gravity contributing an R0 cosmological-like term. The structure of three horizonlike surfaces, viz. timelike limit surface, apparent horizon and event horizon, are determined. We demonstrate the existence of an additional cosmological horizon, in f(R) gravity model, apart from the regular black hole horizons that exist in the analogous general relativity case. In particular, the known stationary Kerr-Newman black hole solutions of f(R) gravity and general relativity are retrieved. We find that the timelike limit surface becomes less prolate with R0 thereby affecting the shape of the corresponding ergosphere.

Shadow of charged rotating black hole surrounded by perfect fluid dark matter

Farruh Atamurotov 2, 3, ∗ and Uma Papnoi 5, † Inha University in Tashkent, Ziyolilar 9, Tashkent ... more Farruh Atamurotov 2, 3, ∗ and Uma Papnoi 5, † Inha University in Tashkent, Ziyolilar 9, Tashkent 100170, Uzbekistan Akfa University, Kichik Halqa Yuli Street 17, Tashkent 100095, Uzbekistan Ulugh Beg Astronomical Institute, Astronomy St. 33, Tashkent 100052, Uzbekistan Gurukul Kangri (Deemed to be University) Vishwavidyalaya, Haridwar 249404, Uttarakhand, India Kanoria PG Mahila Mahavidyalaya, Jaipur 302004, Rajasthan, India

Shadow and deflection angle of charged rotating black hole surrounded by perfect fluid dark matter

Classical and Quantum Gravity

We analysed the shadow cast by charged rotating black hole (BH) in presence of perfect fluid dark... more We analysed the shadow cast by charged rotating black hole (BH) in presence of perfect fluid dark matter (PFDM). We studied the null geodesic equations and obtained the shadow of the charged rotating BH to see the effects of PFDM parameter $\gamma$, charge $Q$ and rotation parameter $a$, and it is noticed that the size as well as the shape of BH shadow is affected due to PFDM parameter, charge and rotation parameter. Thus, it is seen that the presence of dark matter around a BH affects its spacetime. We also investigated the influence of all the parameters (PFDM parameter $\gamma$, BHs charge $Q$ and rotational parameter $a$) on effective potential, energy emission by graphical representation, and compare all the results with the non rotating case in usual general relativity. To this end, we have also explored the effect of PFDM on the deflection angle and the size of Einstein rings.

$Research paper thumbnail of Optical and thermodynamic properties of a rotating dyonic black hole spacetime in $${\mathcal {N}} = 2, U(1)^2$$ gauged supergravity$

Optical and thermodynamic properties of a rotating dyonic black hole spacetime in $${\mathcal {N}} = 2, U(1)^2$$ gauged supergravity

The null geodesics and the distance of closest approach for photon around a rotating dyonic black... more The null geodesics and the distance of closest approach for photon around a rotating dyonic black hole in N = 2, U(1) gauged supergravity is studied. The phenomenon of black hole shadows with various black hole parameters has also analyzed. Further, the investigation of various thermodynamic properties for this black hole is performed with various thermodynamic parameters at the horizon. The heat capacity to study the thermodynamic stability of this black hole spacetime is also studied. The influence for different values of the black hole parameters ν, e, ν, g and Ng on the phenomenon of black hole shadows and thermodynamic parameters is also investigated visually.

Strong gravitational lensing in 5D Myers-Perry black hole spacetime

We study the motion of massless test particles in a five dimensional (5D) Myers-Perry black hole ... more We study the motion of massless test particles in a five dimensional (5D) Myers-Perry black hole spacetime with two spin parameters. The behaviour of the effective potential in view of different values of black hole parameters is discussed in the equatorial plane. The frequency shift of photons is calculated which is found to depend on the spin parameter of black hole and the observed redshift is discussed accordingly. The deflection angle and the strong deflection limit coefficients are also calculated and their behaviour with the spin parameters is analysed in detail. It is observed that the behaviour of both deflection angle and strong field coefficient differs from Kerr black hole spacetime in four dimensions (4D) in General Relativity (GR) mainly due to the presence of two spin parameters in higher dimension.

Thermodynamics from field equations for charged radiating rotating black hole near horizon

International Journal of Modern Physics A

It is well known that near horizon black hole space–times show a resemblance to thermodynamic sys... more It is well known that near horizon black hole space–times show a resemblance to thermodynamic systems, it is easy to associate the thermodynamic parameters like temperature and entropy with them. In this paper, we study the connection between gravitational dynamics of the horizon and thermodynamics for the case of charged radiating rotating axially symmetric black holes. It is shown that Einstein field equation near apparent horizon can be interpreted in the form of thermodynamic law, i.e. [Formula: see text].

Strong lensing and observables around 5D Myers–Perry black hole spacetime

Modern Physics Letters A

We study the motion of massless test particles in a five-dimensional (5D) Myers–Perry black hole ... more We study the motion of massless test particles in a five-dimensional (5D) Myers–Perry black hole spacetime with two-spin parameters. The behavior of the effective potential in view of different values of black hole parameters is discussed in the equatorial plane. The frequency shift of photons is calculated which is found to depend on the spin parameter of black hole and the observed redshift is discussed accordingly. The deflection angle and the strong deflection limit coefficients are also calculated and their behavior with the spin parameters is analyzed in detail. It is observed that the behaviors of both deflection angle and strong field coefficient differs from Kerr black hole spacetime in four dimensions in General Relativity (GR), which is mainly due to the presence of two-spin parameters in higher dimension.