## 1 Introduction  
Mean motion resonance (MMR) or orbital resonance is a common phenomenon both in our Solar system and the exoplanetary system that occurs when there is a ratio of integers between the orbital periods of two objects. For example, a resonance occurs between Neptune and Pluto (3:2 resonance) and Jupiter's moons (1:2:4 resonance) in our Solar system. For MMRs in the exoplanetary system, numerous suspected or confirmed examples exist [1, 2]. The resonant motions in the restricted three-body problem have been studied many times in the past years. The resonant periodic families and their stability corresponding to first-, second-, and other higher-order resonances in the CRTBP and the ERTBP model are reviewed by [3, 4]. The transition between different resonances is also an interesting problem and has been investigated by many researchers. For example, Oterma, which is Jupiter's comet, can make a rapid transition from the interior, near 3:2 resonance, to the exterior, near 2:3 resonance, with the secondary. This phenomenon of Oterma is called resonance hopping [5]. The dynamical mechanism of the resonance transition and capture of Jupiter's comets is explained by [6, 7, 8]. Resonance transitions associated with the structure of the weak stability boundary are discussed in [9]. Furthermore, investigations about the resonance hopping effect are also conducted in the Neptune-Planet Nine system [10]. Recently, studies [11, 12] examined the natural divergence of the first-order resonances for nearly circular orbits at low eccentricities. They indicate the existence of 'bridges' between adjacent first-order resonances at low eccentricities that smoothly connect the apocentric libration zone of a first-order resonance and the pericentric libration zone of the neighboring first-order resonance. This phenomenon is also present with the periodic orbits method in this work. Investigations of these bridges and gaps at low-eccentricity first-order resonance under dissipative effects are presented in [13]. In this paper, we conduct an investigation about the breakup of the first-order resonant periodic families by increasing the mass parameter \(\mu\). In the chaotic region where the 1:1 resonance overlaps with nearby first-order resonances, specific periodic orbits with part of their trajectories resembling an interior/exterior resonant orbit and part of their trajectories resembling another interior/exterior resonant orbit are found, which are called the resonance transition periodic orbits (_RTPOs_). The breakup of the first-order resonance with the increasing mass parameter \(\mu\) and recombination with the resonance transition periodic families (_RTPFs_) are introduced in this paper. In recent years, the application of the resonance phenomenon has attracted much interest in engineering and mission design [14; 15; 16; 17; 18; 19; 20; 21]. Practical missions using the resonant periodic orbits already exist. For example, in the extension phase of the IBEX (Interstellar Boundary Explorer) mission, the spacecraft was maneuvered into an orbit that is in the 3:1 resonance with the Moon [22; 23]. Another mission is the TESS mission (Transiting Exoplanet Survey Satellite), which is in an orbit in the 2:1 resonance with the Moon [24; 25]. By choosing a proper phase with the Moon, this resonant periodic orbit can minimize the radiation dose and avoid long eclipses to improve the efficiency of scientific work and sustain long-term stability. The resonant periodic orbits along with the _RTP_Os investigated in this work may have a wide application for tour missions in the Earth-Moon and other planetary systems in the future. The remainder of this paper is structured as follows. In Section 2, the model framework is introduced. The structures of the first-order resonant periodic families are introduced in Section 3. The breakup and recombination process of the _RTPFs_ with the first-order resonant periodic families are introduced in Section 4.