Black holes (BHs) are considered one of the most distinctive attributes of strong gravitational fields in the present arena of research. Classically, nothing can get away (either particles or radiations) from the event horizon of a BH due to strong gravitational influence. However, it swallows everything found in the surroundings. These thermodynamic entities not only characterize some remarkable classical insights but also come up with a better perception of their quantum gravitational features. The well-known BH configurations, including Schwarzschild, Reissner–Nordstrom (RN) o ̈ , Kerr, and Kerr–Newman, have curvature singularity beyond their event horizons. The quantum mechanical consequences endorse the ejection of thermal radiations from BHs, known as Hawking radiations (Hawking, 1975). These radiations cause a gradual drop in the mass of BH, thus leading to its evaporation, but tend to increase its temperature radically. Hence, thermal radiations play an astonishing role in the thermodynamic aspects of smaller BHs due to a significant increase in temperature. The discovery of Hawking radiation reveals that BHs have a temperature. The entropy and the temperature of BHs indicate that the rules of BH and classical thermodynamics are connected. Specifically, temperature and surface gravity are interrelated, while energy is connected to the BH mass. Entropy is crucial for analyzing the thermal properties of a thermodynamic system and is connected to the field ofBH’s event horizon (Bekenstein, 1973). This similarity argues that, for the second law of thermodynamics to not be violated, the BH entropy must be higher than that of some other object with a volume similar to that of BH. Thus, it is not possible to attain thermal equilibrium between BH and thermal radiations, illustrating the requirement for logarithmic corrections derived from the thermal fluctuations in the entropy area relation provided by Bekenstein (More, 2005).

One of the primary issues with the classical Maxwell theory is the appearance of an infinite self-energy for a point-like charge at the charge position. In quantum electrodynamics, this divergence can be eliminated, but it still presents a challenge in classical electrodynamics. To resolve this issue, Born and Infeld developed a novel Lagrangian (Born and Infeld, 1934). Other nonlinear electrodynamic fields, such as the logarithmic, exponential, and power law Maxwell fields, have drawn greater attention than Born–Infeld nonlinear electrodynamics (NED) (Hendi et al., 2015; Dehghani, 2016; Dayyani et al., 2017; Dehghani and Hamidi, 2017). These theories, which can be reduced to linear Maxwell theory, are more complex than linear electrodynamics. In the existence of nonlinear electrodynamic impacts, Balart and Vagenas (2014) gave the exact solutions of a variety of regularly charged BHs and showed that the behavior of some BHs coincides asymptotically with that of RN BH. Studying the thermal properties of four regular BHs, Tharanath et al. (2015) discovered a second-order phase transition. Inferring the leading-order corrections to thermodynamic quantities of RN, Kerr, and charged anti-de-sitter (AdS) BHs, Faizal and Khalil (2015) concluded that these BHs produce remanence in all three cases. In an attempt to better understand the local thermal stability and logarithmic entropy adjustments of charged accelerating BHs, Pradhan (2019) detected second-order phase transitions in these BHs. According to the investigation of Sharif and Akhtar (2020)into the impact of thermal fluctuations on the thermodynamics of charged BHs with Weyl corrections, tiny BHs are unstable when logarithmic corrections are included. The stability and thermodynamics of asymptotically flat RN BH were examined by Sinha (2021). Additionally, he noted that BH displays a phase transition that is distinct from that of the Schwarzschild BH. Javed et al. (2023) studied thin-shell wormholes and gravastars in the background of different BH geometries.

The impact of logarithmic corrections on the thermodynamic variables such as heat capacity, Hawking temperature, and entropy of the modified Hayward BH was discussed by Pourhassan et al. (2016). In the presence of the cosmological constant, Jawad and Shahzad (2017) examined thermodynamic stability and the impact of thermal fluctuations on the non-minimal regular BHs. They concluded that normal BHs exhibit stable behavior for increasing cosmological constant values. The thermodynamic characteristics of the Hayward and the asymptotically AdS BHs under equilibrium conditions were investigated by Haldar and Biswas (2018) to an impact of thermal disturbances. Saleh et al. (2018) observed that the presence of the magnetic charge and quintessence produces the phase transition in regular BH after analyzing the behavior of thermal quantities such as heat capacity and temperature of Bardeen BH surrounded by quintessence. Javed et al. (2018) studied the thermodynamic characteristics and phase transition of regular charged BHs. They discovered that for charged BH with exponential distribution of variables, the phase transition curves diverge around critical points. Sharif and Nawaz (2020) explored the thermodynamic features of rotating regular BHs and their AdS versions and concluded that considered BHs are thermodynamically more stable and less hot than ordinary Kerr and Kerr-AdS BHs. Sharif and Ama-Tul-Mughani (2021) discussed the phase transition of the Kerr-Sen-AdS BH and concluded that BH attains the same phase transition as that of liquid–gas van der Waals fluid. They also analyzed how thermal fluctuations impact the stability of the considered BH. Sharif and Khan (2022a) studied how thermodynamic properties, thermal stability, and logarithmic correction impact on thermodynamic quantities and phase transitions of regular de Sitter BH. They demonstrated that the phase of Hawking’s temperature varies from positive to negative, whereas the phase of heat capacity varies from negative to positive for greater values of the de Sitter parameter.

The generalization of thermodynamic analogy between the van der Waals system and AdS BH is the Joule–Thomson expansion process. According to classical thermodynamics, the Joule–Thomson expansion describes how a fluid moves from an area with high pressure into a low-pressure area through a porous plug while maintaining a constant enthalpy. Ökcü and Aydýner (2017) examined the charged RN AdS BH’s Joule–Thomson expansion in the extended phase space. They discovered the inversion/isenthalpic curves and the cheating/cooling regions. This groundbreaking research has since been applied to a variety of different BHs, including the quintessence-charged AdS BH (Ghaffarnejad et al., 2018), the Kerr-AdS BH (Ökcü and Aydýner, 2018), the d-dimensional charged AdS BH (Mo et al., 2018), the holographic superfluid (D’Almeida and Yogendran, 2018), the charged AdS BH in f(R) gravity (Chabab et al., 2018), the charged AdS BH with a global monopole (Rizwan et al., 2018), the charged AdS BH in Lovelock gravity (Mo and Li, 2018), and the charged Gauss–Bonnet BH (Lan, 2018). Pacilio and Brito (2018) examined the QNMs of weakly charged Einstein–Maxwell dilaton BHs and found that gravitational modes are only weakly affected by coupling with the dilaton. The QNMs and quantization were studied for the analytical solutions in a cosmic string Born–Infeld dilaton BH geometry in Sakalli et al. (2018). Greybody factors of modified BH geometry in the background of NEDs were studied in Kanzi et al. (2020). QNMs, photon spheres, and shadows of regular BH with string cloud parameters were discussed in Singh et al. (2022). Nomura and Yoshida (2022) investigated the QNMs of charged BHs with corrections from NEDs and found that the isospectrality of QNMs under parity is generally violated due to NEDs.

Thermal stability with emission energy and Joule–Thomson expansion of regular BTZ-like BH are studied in Ditta et al. (2022) and tunneling analysis of null aether BH in Ali et al. (2022). The thermodynamics of accelerating BHs in ADS spacetime were discussed in Anabalon et al. (2018). The effects of NED on the BH shadow, deflection angle, quasinormal modes (QNMs), and graybody factors are calculated in Kuang et al. (2018) and Okyay and Övgün (2022). QNMs are observed for hairy BHs in (Yang et al., 2022a), QNMs of f(Q) BH are examined in Gogoi et al. (2023), and Kerr-like black bounce spacetime is calculated in Yang et al., (2022b); Övgün et al., (2021). The deflection angle of the photon, QNMs, the greybody factor, and shadows were discussed in Övgün (2018), Övgün and Jusufi (2018), Javed et al. (2019), and Pantig et al. (2022). Guo et al. (2020) examined the Joule–Thomson expansion for the regular AdS BH and determined the inversion temperature for Bardeen-AdS BH in the extended phase space. They analyzed the inversion and isenthalpic curves for the BH under consideration and found that their intersection points are the inversion points discriminating the cooling from the heating process. Gracia et al. (2021) studied this expansion for uncharged noncommutative BHs characterized by a parameter (present in the horizon function) and found that the uncharged BH in a noncommutative scenario acts as a charged commutative BH.

In this study, we explore the thermodynamic features and QNMs of charged ADS BH with NED. This study is devoted to exploring the effects of NED on thermodynamic quantities of charged ADS BH geometry. It is outlined as follows: Section 2 presents the charged ADS BH structure with NED and discusses the thermodynamic quantities and thermal stability through heat capacity, Section 3 discusses the rate of emission energy of the considered BH geometry, and Section 4 explains the relationship between the QNMs and Davies’s point. The consequences of thermal fluctuations on uncorrected thermodynamic physical quantities are examined in Section 5. In the last section, we present some concluding remarks.

The following action is described as the minimal interaction between NED and gravity (Yu and Gao, 2020): S = ∫ Y ψ + R − g 16 π d 4 x , (1) where F γ β = ∇ γ A β − ∇ β A γ , ψ = F γ β F γ β , γ , β = 0,1,2,3 , where R is the Ricci scalar, A _γ denotes the Maxwell field, and Y[ψ] is a function of ψ. By varying the aforementioned action, the corresponding field equations result in Yu and Gao (2020): G γ β = 1 2 g γ β Y ψ − 2 Y ψ , ψ F γ μ F β μ , (2) where Y [ ψ ] , ψ = d Y [ ψ ] d ψ .The associated generalized Maxwell equations are provided as ∇ γ Y ψ , ψ F γ β = 0 . (3)

The parameterizations of the spherically symmetric static spacetime are d s 2 = − B r d t 2 + B − 1 r d r 2 + r 2 d θ 2 + r 2 ⁡ sin 2 ⁡ θ d ϕ 2 . (4) Here, the metric function is denoted as B ( r ) . The respective non-zero component of the Maxwell field tensor is A ₀ = ϕ(r) and ψ = −2ϕ′².

Now, we consider a specific expression of Y [ ψ ] = − 2 2 β − ψ + ψ + 2 Λ , where the coupling constant is denoted as β and the corresponding solution of field equations is (Yu and Gao, 2020) ϕ r = − q / r − r β , (5) B r = − 2 M r + 2 β Q + Q 2 r 2 − β 2 r 2 3 + 1 − 1 3 Λ r 2 , (6) where Λ, Q, and m are the cosmological constant, charge, and mass of BH geometry, respectively. Here, we consider the following choices of physical parameters Q and β, and the respective manifolds become as follows:

• If β = 0 = Q, then Schwarzschild-ADS BH is recovered.

It is interesting to mention that the BH event horizon is located at a radial position for which the metric function becomes 0. In Figures 1–3, we discuss the behavior of the metric function for suitable values of physical parameters. It is noted that the position of the event horizon (dashed line B ( r ) = 0 ) in between the shaded regions depends on β, M, and Q. It is interesting to mention that BH event horizon shows symmetric behavior for different values of coupling constant. (Figure 1). The position of the event horizon becomes larger as the coupling constant approaches 0 (β ⇒ 0). As the charge of the BH geometry increases, the range of coupling parameters of the event horizon also enhances. Conversely, there is a small possibility of an event horizon of charged BH with NED for only 0 < Q < 0.2 at β = 0.4, whereas for higher values of β, the ranges of charge the existence of event horizon increase (Figure 2). The possible existence of an event horizon depends on the charge and the coupling constant. The inner and outer horizons of charged ADS BH with NED depend on the cosmological constant (Figure 3).

Here, we are interested in evaluating the Hawking temperature heat capacity of the considered BH spacetime. Such thermodynamic entities play a crucial role in exploring the thermodynamically stable characteristics of BH. The respective mass of BH in terms of the event horizon is given as M = 3 Q 2 + 6 β Q r h 2 + r h 4 − β 2 + Λ + 3 r h 2 6 r h , (7)

The surface gravity κ = 1 2 d B ( r h ) d r h of BH has the following form: κ = M r h 2 − Q 2 r h 3 − β 2 r h 3 − Λ r h 3 . Consequently, we get the Hawking temperature T = κ 2 π as (Hawking, 1975) T = M 2 π r h 2 − Q 2 2 π r h 3 − β 2 r h 6 π − Λ r h 6 π . (8)

Figure 4 analyzes the behavior of the Hawking temperature in terms of the entropy of BH geometry. The left plot shows that the temperature of the system greatly depends on the mass of the geometry. It is noted that temperature increases initially and then decreases as the entropy of the system increases. In the background of the cosmological constant, the Hawking temperature enhances compared to the charged BH with NED in Figure 5.

By considering the Bekenstein area entropy relationship, the entropy of the system is given as (Das et al., 2002) S = ∫ 0 2 π ∫ 0 π g θ θ g ϕ ϕ d θ d ϕ = π r h 2 . (9) The heat capacity T ∂ S ∂ T of the system has the following form (Das et al., 2002; Sharif and Khan, 2022b): C = 2 π r h 2 − 3 M r h + 3 Q 2 + r h 4 β 2 + Λ 6 M r h − 9 Q 2 + r h 4 β 2 + Λ . (10)

The divergence point of the heat capacity is referred to as Davies’s point, which plays an important role in discussing the thermodynamic stability of the BH structure. Davies’s point is also known as the phase change point from negative to positive or positive to negative. It is noted that the positive region before the Davies point shows a stable region, and the negative region after the Davies point represents an unstable region (Das et al., 2002; Sharif and Khan, 2022b). Hence, the radial position of BH at which it changes the phase is given where r _DP is represented by the position of Davies point.

Figure 6 is used to discuss stable and unstable configurations using the Davies point of heat capacity of BH. In the absence of β and Q (as Schwarzschild-ADS BH), the BH structure shows an unstable configuration, while for non-zero values of β and Q, the system shows a stable configuration for smaller BHs. It is also noted that the stable configuration is increased for higher values of β. Hence, the presence of NED-charged BH shows a stable configuration for smaller ADS BHs, while larger ADS BH shows unstable behavior.

The formation and destruction of an excessive number of particles very close to the horizon are known as emission energy, and quantum fluctuations in the interior of BHs are the source of this energy. The main reason for the BH evaporation within a certain period is due to the positive-energy particles that tunnel out of the BH in the core area where Hawking radiation occurs. Here, we are interested in exploring the energy emission rate associated with the considered BH geometry with NED. At very high energy, the absorption cross-section often oscillates around a limiting constant value σ _lim . The limiting value of σ _lim is related to the radius of the event horizon (Wei and Liu, 2013; Papnoi et al., 2014; Eslam Panah et al., 2020): σ lim ≈ π r h 2 . (11) The respective expression of the rate of BH energy emission becomes (Wei and Liu, 2013; Papnoi et al., 2014; Eslam Panah et al., 2020) d 2 ε d ω d t = 2 π 2 σ lim exp ω T − 1 ω 3 , (12) and by considering the Hawking temperature T of the considered BH, we get d 2 ⁡ ε d ω d t = 2 π 3 r h 2 ω 3 exp − 6 π r h 3 ω − 3 M r h + 3 Q 2 + r h 4 β 2 + Λ − 1 . (13)

Figure 7 shows the behavior of the rate of emission energy along the frequency with suitable values of physical parameters. It is found that the energy rate increases as frequency gradually increases initially, approaches its peak value, and then decreases. It is concluded that the rate of emission energy decreases for higher values of charge and NED parameter.

Here, we are interested in calculating the null geodesics and radius of the photon sphere of charged ADS BH with NEW. Then, we determine the photon angular velocity and Lyapunov exponent using photon radius.

Here, we discuss the effects of thermal fluctuation on the charged ADS BH with NED. For this purpose, we find the mathematical expression of the corrected entropy of the system using the partition function defined as follows (Pourhassan et al., 2018; Pradhan, 2019; Sharif and Khan, 2022b): R ξ = ∫ 0 ∞ ρ E exp − ξ E d E , (23) where the density state is denoted with ρ(E) and the average energy is E. The density state is evaluated using the inverse Laplace transformation of the previously defined function given as ρ E = 1 2 i π ∫ − i ∞ + ξ 0 i ∞ + ξ 0 ⁡ exp ξ E R ξ d ξ = 1 2 i π ∫ − i ∞ + ξ 0 i ∞ + ξ 0 ⁡ exp S ̃ ξ d ξ , (24) where the exact corrected expression of entropy is S ̃ ( ξ ) = β E + ln ⁡ Z ( ξ ) with ξ > 0. By considering Taylor series expansion of ξ ₀, we get S ̃ ξ = S + 1 2 ξ − ξ 0 2 ∂ 2 S ̃ ξ ∂ ξ 2 ξ = ξ 0 + O ξ − ξ o 2 . (25) The equilibrium entropy S satisfies the relations ∂ S ∂ ξ = 0 and ∂ 2 S ∂ ξ 2 > 0 . Using Eq. 25 in Eq. 24, we obtain ρ E = 1 2 π i exp S ∫ d ξ ⁡ exp 1 2 ξ − ξ 0 2 ∂ 2 S ̃ ξ ∂ ξ 2 . (26) Furthermore, it yields (Pourhassan et al., 2018; Pradhan, 2019; Sharif and Khan, 2022b) ρ E = 1 2 π exp S ∂ 2 S ̃ ξ ∂ ξ 2 ξ = ξ 0 − 1 2 , (27) which becomes S ̃ = S − 1 2 ln S T 2 + η S . (28)

We may use a broader parameter χ without losing generality, except for the factor 1 2 , which increases the influence of correction terms on the entropy of BH. The corrected entropy may be expressed in this context as follows (Sharif and Khan, 2022b): S ̃ = S − γ ⁡ ln S T 2 + η S . (29) By considering alternative correction parameter values γ and η, we obtain

• Uncorrected entropy (UCE) ⇒ if η, γ → 0.

Figure 10 shows the graph of corrected entropy through four different cases as UCE, SLCs, SOCs, and HOCs for Schwarzschild-ADS (first plot), RN-ADS (second plot), and charged ADS BH with NED (third and fourth plots). It is noted that for all cases, system entropy is monotonically increasing throughout the considered domain for larger BHs. It is noted that the graph of usual entropy is increasing smoothly (left plot blue curve), but the corrected expression fluctuates for smaller BHs, increasing smoothly for larger ones. Thus, these correction terms are more effective for small BHs. The corrected entropy shows the larger behavior for the case of HOCs.

Now, we consider the expression of corrected entropy to explore the corrected energies of the considered BH solution. Under thermal fluctuations, the modified first rule of BH thermodynamics may be expressed as follows (Jawad and Shahzad, 2017; Sharif and Khan, 2022b): d M = T d S ̃ + V d P + Φ d Q + Ψ d β , (31) where T denotes the corrected Hawking temperature. In this case, Φ and Ψ are the new conjugate quantities and Q and β are new thermodynamic variables. The relations can be used to derive these potential functions: T = ∂ M ∂ S ̃ Q , P , β , V = ∂ M ∂ P T , Q , β , Φ = ∂ M ∂ Q T , P , β , Ψ = ∂ M ∂ β T , Q , P which turns out to be T = π r h Q − β r h 2 2 + Λ r h 4 − r h 2 − 3 M r h + 3 Q 2 + r h 4 β 2 + Λ 4 η − 3 M r h + 3 Q 2 + r h 4 β 2 + Λ − π 2 r h 4 − 3 M r h + 3 Q 2 + r h 4 β 2 + Λ + π γ r h 2 3 M r h − 6 Q 2 + 2 r h 4 β 2 + Λ , Φ = − 3 r h 6 M + r h r h 2 4 β 2 + Λ − 3 Q − β r h 2 2 + Λ r h 4 − r h 2 2 r h 2 − 6 β r h r h 6 M + r h r h 2 4 β 2 + Λ − 3 + 3 3 M + 3 r h 2 r h 2 4 β 2 + Λ − 3 , Ψ = − r 3 r h 4 r h r h − 2 M + 4 Q 2 − Λ r h 8 Q − β r h 2 2 + Λ r h 4 − r h 2 6 − 2 Q 3 r h 4 r h r h − 2 M + 4 Q 2 − Λ r h 8 + r h 3 r h − 3 M + 8 Q 2 r h 2 , V = 4 π r h 3 3 . When the foregoing expressions are substituted in Eq. 31, the modified first law of BH is verified, suggesting that the existence of thermal fluctuations enhances the reliability of the first law of BH thermodynamics.

This study is devoted to exploring the thermodynamics of charged ADS BH with NED through QNMs and thermal fluctuations. We explore the effects of NED parameter β on the thermodynamic quantities of charged ADS BH. Some important features of the present study are itemized as follows:

• The graphical behavior of the lapse function under the effect of involved model parameters is provided in Figures 1, 2. The position of the event horizon depends on the charge and the coupling constant β.

Hence, to sum up, it is determined that the cosmological constant and NED greatly affect the thermodynamic properties of charged ADS BHs.