The merger of hard binaries in globular clusters as the primary channel for the formation of second generation stars.

The crucial role of binary-mediated collision/merging of G1 stars in the formation of (the bulk of) G2 stars in GCs implies that it is a binary consuming process. Hence, one may expect a relationship between the observed binary fraction and the population of G1 stars. Figure 1 displays the dependence of the parameter ($N_{\rm G1}/N_{\rm tot}$), the fraction of G1 stars, on f(q$>0.7$), the fraction of binaries with the mass ratio q$>0.7$ in GCs of the sample. In the middle panel of Figure 1, the parameter ($N_{\rm G1}/N_{\rm tot}$) is plotted as a function of the logarithm of f(q$>0.7$). The continuous line in the middle panel is a linear fit to the data. The plot in the right panel of Figure 1 shows the parameter ($N_{\rm G1}/N_{\rm tot}$) as a function of the ratio between the fractions of binaries with different mass ratios, f(q$>0.7$) and f(q$>0.5$). This dependence is discussed in detail in Subsection 3.2 along with a summary of closely related relevant results obtained and accumulated to date on binary stars.

We estimated the level of statistical significance of the dependencies shown in Figure 1. The results of the Spearman’s rank correlation test done to assess the correlation between the data sets plotted in Figure 1 are listed in Table 1. As can be seen, the correlation is statistically significant at very high confidence level for the same dependence shown in two forms (left and middle panels). We made separate estimates for both forms of the dependence in order to take care of a formality. The significance of the trend in the right panel was estimated for two its versions, the total and reduced. The reduced version is coded by magenta color in Figure 1. It is obtained by reducing from the total set of data (45 units) 10 GCs (22% of the sample) with the largest errors of the ratio f(q$>0.7$)$/$f(q$>0.5$). These points make the trend more diffuse and somewhat less significant according to the test. The reduced version of the trend is surely significant at a high confidence level of 99.91% as compared to somewhat lower confidence level of 97.07% for the total data set.

These dependencies provide another piece of evidence supporting our scenario. First, the fraction of MS binaries is proportional to the fraction of G1 stars in GCs or, in other words, this means that the smaller fraction of binary stars in GCs, the larger, on average, the fraction of G2 stars. A systematically decreasing fraction of binaries in GCs with systematically increasing fraction of G2 stars may be explained as due to the formation of G2 stars from binaries. However, it is known (Milone et al., 2012) that GCs with larger fraction of binaries are also systematically more massive. So, the discussed relation may alternatively be interpreted as being due to more efficient disruption of binaries in more massive GCs. The trend presented in the right panel of Figure 1 does not support the latter interpretation. The trend shows that the smaller the fraction of G1 stars is, the more deficient binaries of higher mass ratio (q$>0.7$) are. These binaries of higher mass ratio are, on average, harder than their smaller mass-ratio counterparts due to higher binding energy at a given primary mass. In the next Subsection, we justify this in detail.

This subsection deals with the subject of the most suitable and probable kind of binaries that could primarily be involved in the (trans)formation of (G1 into) G2 stars. The dependence of ($N_{\rm G1}/N_{\rm tot}$) on the binary fraction ratio (right panel, Figure 1) implies that it is their fraction with q$>0.7$ of the mass-ratio distribution. Indeed, this dependence unambiguously shows that the relative fraction of the higher mass-ratio binaries decreases with decreasing fraction of G1 RGB stars in GCs. Virtually the same binaries are expected to be the hardest in GCs at a given primarily mass. Strictly speaking, the data on the fractions of MS binary stars of different mass ratio in GCs used in our analysis do not allow one to distinguish between soft and hard binaries. So, one cannot directly refer to the kind of these binaries, as soft or hard. Then, do we have any ground to relate the obtained dependencies with our approach? In other words, may we interpret the formally decreasing amount of binaries with decreasing fraction of G1 stars in GCs as probably due to the transformation of the binaries into G2 stars rather than to the disruption of a larger number of binaries in GCs with smaller ($N_{\rm G1}/N_{\rm tot}$)? Of course, the issue is really complex. Nevertheless the trend in the right panel of Figure 1 supports such an interpretation, given a body of both observational and theoretical present-day data about binaries and multiple systems. In order to explain this trend, we briefly summarize key actual data on binary stars and their characteristics appropriate to the case, particularly on hard (close) binaries, their probable mass-ratio distribution and their fate in GCs.

According to the present-day understanding of the issue, the dynamical evolution of binaries (triples) in GCs develops in two opposite ways, namely: dynamically hard and soft binaries become even harder and softer, respectively (e.g., Spera et al., 2022; Rozner & Perets, 2022, and references therein). Thus, dynamically soft binaries can hardly survive for a long time in the high-density environment of GCs. In particular, both tidal disruption by the gravitational potential of GCs and dynamical evaporation tend to soften and finally disrupt these binaries (Rozner & Perets, 2022). Therefore, a fraction of the initially formed binaries, primarily soft ones, are expected to be essentially disrupted, while on the other hand, hard binaries increase their binding energy. There is a well known complexity of the effects on hard binaries in the condition of high-density environment due to their interactions with other GC constituents, such as single stars, other binary stars, and black holes. A part of their increasing binding energy is lost to kinetic energy of escaping single stars. Also, one cannot exclude that hard binaries achieving a threshold binding energy can eject themselves before merging. Nevertheless, despite these effects, the most probable development and the fate of the dynamical evolution of hard binaries in GCs is expected to be merger or collision (Goodman & Hut, 1993). Supporting evidence of a similar effect with a lower efficiency is observed among field stars. Tokovinin et al. (2006) established that close spectroscopic binaries with and without tertiary companion have significantly different period distributions whereas their mass-ratio distributions are similar. So, the dynamical effect of such tertiary companions leads to shorter periods of respective binaries. It is now evident that virtually all short-period binary stars in the field have a tertiary companion. In the more general context of the observed relation between close binaries and solar-type hierarchies, Tokovinin (2023) finds that the inner subsystems in these hierarchies show strong excess of periods shorter than 30 days. Interestingly enough, the eccentricities of the same subsystems tend to be zero, and a larger fraction of twins belongs to these short-period binaries, too.

In addition to the dynamical effects making hard binaries become harder in the dense environment of GCs, with their probable fate being a merger, there may be other potential effects favoring the merging of binaries. For instance, Rozner & Perets (2022) argue that the properties of binaries in the early GCs could be affected by the gas produced by the evolved G1 stars. The presence of gas can lead to an efficient merger of binaries, on the one hand, and to the formation of additional population of binaries, on the other.

It is now widely accepted that the mass-ratio distributions of MS binaries in both the field and clusters are in obvious disagreement with random pairing of stars taking their proportions from the IMF into account. Moreover, a body of observational evidence converge towards a particular feature in the mass-ratio distribution of solar-type binaries in the form of a prominent peak (excess) of twin binaries, i.e. with mass-ratio close to unity. We primarily refer just to low-mass, so-called solar-type stars, with the primary mass $0.5-1.5$ M_☉, which are relevant to this study. Fisher et al. (2005) studied a sample of field spectroscopic MS binaries with the primary mass greater than $1.1$ M_☉ and found an evident peak in the mass-ratio distribution near q=1. Using a sample of 454 solar-like (F6–K3) stars from the Solar vicinity, Raghavan et al. (2010) revealed that the mass-ratio distribution shows ”a preference for like-mass pairs”, which are more frequent in relatively close pairs. Tokovinin & Moe (2020) compared their model with observational data on binary stars, namely with a large sample of solar-type binaries obtained by Tokovinin (2014a) within 67 pc from the Sun. They noted that the model reproduces well the large excess of twin binaries (with q$>0.95$), the fraction of which is larger among close binaries (Tokovinin, 2014b). In the old open cluster M67, Albrow & Ulusele (2022) estimated the fraction of photometric binaries with q$>0.8$ to be $\sim$14% (and $\sim$26% with q$>0.5$). From their overview of a variety of observational studies on binary stars including low-mass ones, Pinsonneault & Stanek (2006) argued that there is clear evidence of a typically large fraction of twin binaries (or at least with q$>0.8$) revealed in these works (up to 35% of such binaries).

By proceeding from the observational evidence that close binaries typically have mass ratios close to unity, the so-called twin binaries, Adams et al. (2020) theoretically explained this as being due to the fact that this corresponds to the lowest energy state of such binary systems.

We qualitatively formulate our approach in a more specific form defined by the transformation of high mass-ratio G1 binaries into G2 stars of approximately two times higher mass than the primary one. This means that lower-mass G1 stars forming such twin or almost twin binaries are transformed into a more massive G2 stars, which replace less numerous (in absolute value, but at the same or comparable fraction) G1 binaries at this higher mass, since these latter stars are in turn transformed into even more massive G2 stars. This way, a successive shifting of more numerous (in absolute value) lower-mass stars, transformed into G2 stars, towards two times more massive (and therefore many times less numerous at that mass) G1 stars is a mechanism that can naturally and uniformly operate and lead to similar outcome in different GCs.

We now attempt to obtain more quantitative estimates of how the binary star fraction can relate to the fraction of G1 stars. We use the following arguments. Suppose that the fraction of hard binaries of G1 stars, $f_{\rm B,M}$, corresponding to the number $N_{\rm B,M}$, with both the primarily mass around $M$ and high mass ratio (virtually twins), are transformed into the same number of G2 stars with mass around 2$M$. Similarly, due to the same process, $b$ times larger number of hard binaries with the primary mass around $0.5M$ are transformed into single G2 stars, $N_{\rm S,M}({\rm G2})$, with mass around $M$, while the number of G1 stars left around the same mass $M$ is $N_{\rm S,M}({\rm G1})$. In other words, the transformed $N_{\rm B,M}$ G1 binaries were substituted with $b$ times larger number of G2 stars, $N_{\rm S,M}({\rm G2})$. Then, $N_{\rm S,M}({\rm G2})=bN_{\rm B,M}$. Note that the fraction of hard binaries $f_{\rm B,0.5M}$ is not necessary equal to $f_{\rm B,M}$ in general case, since the fraction of hard MS binaries in a GC may vary along the MS. One can easily qualitatively express the binary fraction $f_{\rm B,M}$ the following way:

Our goal is to approximately estimate a typical realistic value of the parameter $g_{\rm 1}$, the fraction of G1 MS stars around mass $M$, which was defined in Kravtsov et al. (2022) as the analog of the fraction of G1 RGB stars [i.e., $N_{\rm 1}({\rm G1})/N_{\rm tot}=N_{\rm 1}({\rm G1})/(N_{\rm 1}({\rm G1})+N_{\rm 2}({\rm G2}))$]. Taking the above-mentioned expressions into account, $g_{\rm 1}$ is expressed as:

From here and using Equation 1 we easily come to the following expression:

For estimating typical value of $g_{1}$, the value of $b$ may be around $b\approx 5$, i.e. equal to the ratio of the number of single stars, with the given ratio of their mass, defined by the canonical Kroupa IMF (Kroupa, 2001, 2002)¹¹1This value of $b$ can be different if the shape of the IMF is calibrated according to the IMF slope versus stellar surface density of the cluster found by Dib (2023).. Namely, we accept the ratio of their mass is equal to $\approx 2$ and the slope of the IMF is $\alpha=2.3$ in the range of low-mass stars, at $M_{\rm MS}<1.0$ M_☉. Since the fraction of hard, high-mass ratio (virtually twin) binaries that have finally merged in GCs is an obvious variable, we consider two distinct values for it, namely $f_{\rm B,M}=0.10$ and $f_{\rm B,M}=0.30$. They presumably bracket the plausible range for this variable in GCs. Each of the two values is accepted to be constant in the considered stellar mass range, although, in the general case, the fraction of hard (close) binaries may vary with stellar mass as we noted earlier. Then, by applying Equation 3, we obtain the values of $g_{\rm 1}$ equal to 0.64 and 0.32, respectively. This is a reasonable range in comparison with the fractions of the G1 RGB stars, ($N_{\rm G1}/N_{\rm tot}$) that are estimated for most GCs in the Milky Way. However, massive GCs have lower values of ($N_{\rm G1}/N_{\rm tot}$), typically between 0.20 and 0.25. Such values of $g_{\rm 1}$ can be obtained for some useful and interesting cases. In particular, it is worth noting the aforementioned case of $f_{\rm B,M}$ varying along MS, for example, as an increasing function of decreasing stellar mass. This tendency seems to be real at least for the field stars at solar metallicity. For instance, Tokovinin & Moe (2020) note an interesting detail, namely that ”the excess twin fraction is substantially reduced for close early-B binaries and quickly diminishes with increasing separation” in contrast with the same characteristic estimated by the same authors for solar-type stars. In such a case, suppose that the value of $b$ increases, say, up to $b=7$ between the same masses, $0.5M$ and $M$, within $M_{\rm MS}<1.0$ M_☉. Then the value of $g_{\rm 1}$ decreases up to $g_{\rm 1}=0.25$ for $f_{\rm B,M}=0.30$. Note, however, that a detailed analysis of this issue is outside the scope of the present paper.

The mechanism described above for the formation of G2 stars directly suggests that the abundance of light elements (primarily CNO-Na) distinguishing G2 stars from their G1 counterparts, were synthesized in the stellar interiors and transported to the stellar surface. However, this point is very disputable and it suffers from high grade of uncertainty. The formation of a merger-induced G2 MS star as a result of the merger of two G1 MS stars has yet to be investigated in detail. Its particularly challenging step is the formation of one whole hydrogen-burning nucleus from the two merging ones. The merging of G1 stars is accompanied with the transformation of the system angular momentum and with an initially strongly perturbed non-equilibrium state of the merger product. The coalescence of the hydrogen-burning nuclei of G1 stars into one whole nucleus should temporally boost the central temperature and pressure in the forming nucleus as compared to the same parameters in the nucleus of a G1 star of the same mass. As of now, there is unfortunately significant uncertainty about this process and a lack of reliable knowledge about the temporal variations of the central temperature, its maximum possible value achievable at the initial stage of the formation of the merger product. This would have a strong impact on the yields of relevant nuclear reactions. Whether the difference of the CNO-Na surface abundances between G1 and G2 stars can be explained in the framework of our scenario due to the processes generated by low-mass mergers in the interiors of their products is a key question that should be clarified by dedicated numerical simulations. The results obtained so far on the modeling and simulation of the processes related to the mergers of low-mass stars do not exclude or even partially support the ant-correlated variation of the surface abundances of at least some elements. Such a variation of N and C may take place, increasing with time, but emerging at best $\sim 2$ Gyr after the event occurred, depending on the model (Sills et al., 2005).

According to the models of Prantzos et al. (2007), the core H-burning temperature in stars increases towards the end of the MS evolution and it may reach up to $\sim 27\times 10^{6}$K even in low-mass stars with $M_{\rm MS}=0.9$ M_☉ (at [Fe/H]=-1.6). The authors note that this temperature is yet somewhat lower than what is typically required for the NeNa-chain to operate (it becomes sufficient at the RGB, particularly near its tip, where the temperature can exceed $\sim 60\times 10^{6}$K). In their Figure 4 (left panel), Prantzos et al. (2017) indicate the temperature range as a function of the produced He amount ($\Delta Y$, which is used as a proxy for time) where each of the relevant chemical elements is either overproduced (including Na) or depleted with respect to its initial value by the factors corresponding to the extreme abundances observed in the GC NGC 2808 where [Na/Na₀]$>0.7$. The low temperature limit necessary for synthesizing the required amount of Na exactly for this particular case is around $40\times 10^{6}$K at $\Delta Y<0.02$. The lower the value of [Na/Na₀] is, the lower is the temperature limit.

We only briefly note that in the framework of the merger/collision formation of G2 stars, a qualitative interpretation of the disappearing Mg-Al anti-correlation in less massive or most metal-rich GCs can be considered in terms of the expected impact of decreasing velocity dispersion and increasing viscosity of the stellar matter, respectively. Indeed, the kinetic energy of colliding/merging H-burning nuclei apparently depends on the two factors at a given stellar mass.

In this context, it is important to point out to another interesting advantage of the merger-induced scenario for the formation of G2 stars as compared with their canonical formation from H-processed material ejected by polluters (and diluted with pristine gas with composition of G1 stars). The former mechanism requires an order of magnitude less amount of the enriching material to form the same amount (i.e., the same total mass) of G2 stars with a given chemical composition. The main reason is that this difference is defined by the much lower efficiency of star formation of the canonical mechanism. It can hardly be more than 20% as compared with the almost 100% efficiency ($\sim$90%) of the merger-induced mechanism. In other words, this mechanism requires to synthesize, say, at least 5 times less amount of the required chemical elements. This directly implies an apparently lower required rate of the involved nuclear reactions corresponding to a lower temperature limit. Whether the central temperature could temporally achieve or even exceed the minimum required level in a forming low-mass merger/collision products of $M_{\rm MS}=0.8-0.9$ M_☉ (the bulk of the available spectroscopic data on the O, Na, Mg, Al abundances in GCs were obtained in GCs for RGB stars) is one of the key question that have yet to be answered.

In contrast to the high degree of uncertainty of the possibility for the necessary amount of material to be processed at least through the CNO cycle and the NeNa chain in low-mass MS collision products, the availability of a mechanism capable of transporting such a material to the external parts of these products (MS G2 stars) looks very likely. Indeed, the effects of rotation in the interiors of collision products are theoretically known more reliably, with lower degree of uncertainty. Collision products are expected to be fast rotators at least in the initial period after their formation. Lombardi et al. (1996) used smoothed particle hydrodynamics simulations of stellar collisions between MS stars in GCs and noted that any off-axis collisions result in rapidly, differentially rotating merger remnants. Later, Sills et al. (2005) confirmed that these off-axis collision products have substantial angular momentum from their initial configuration (even assuming initially non-rotating stars). Moreover, Sills (2015) noted that very high initial rotation rates of the collision products must be reduced by an unknown process to allow these products to collapse to the MS. So, rotational mixing is the very likely mechanism that would transport the yields of the assumed CNO cycle to the stellar surface. This process and its impact on the variation of the surface elemental abundance of collision products is considered, in particular, in the models of low-mass collision products by Sills et al. (2005). Their models show, for example, essential variation of the surface abundance of N (in excess) and C (in depletion). Add also that one of the main effects of tides in close binaries is that they tend to spin-up the companions and this tidal spin-up establishes rotational mixing in the stellar interiors of the companions before their merging (Spera et al., 2022).

The proposed mechanism of the formation of G2 stars not only avoids the problematic mass budget problem common to other alternatives, but also it apparently does not need an external primordial gas for dilution. We have to note, however, that according to Prantzos et al. (2007), in the case of the dilution of Li-free gas processed through the CNO cycle at high temperature in the polluters (which are massive or intermediate-mass stars in the scenarios relying on the canonical formation of G2 stars, though), the situation is different, i.e. ”the unprocessed material has to be of pristine nature (i.e. pure ISM) rather than from the stellar envelope of the polluter itself”.

On the other hand, rotational mixing, as the main mechanism responsible for the variation of the surface elemental abundances of merger products, should not lead to an essential depletion in the surface lithium abundance of the merger products (G2 stars). Strassmeier et al. (2012) find that binaries exhibit, on average, approximately 0.25 dex less surface Li than single stars of comparable temperature, as expected if the depletion is due to the rotation. In turn, Aguilera-Gómez et al. (2023) find no evident impact of binarity on Li abundance among field RGB stars of their sample. Even more so Sayeed et al. (2023) find a larger fractions of fast rotators among Li-rich stars. The issue of Li abundance in low-mass stars, enriched by numerous observational results for the last years, is contradictory and even surprising. Recent studies of low mass-stars sometimes show paradoxical results on Li abundance. Sayeed et al. (2023) find that Li-rich stars at the base of the RGB have somewhat higher mean s-process abundances and confirm a prevalence of Li-rich stars on the red clump, i.e. among core helium-burning red giants. Surprising enough that this enrichment with Li, not predicted by a standard evolution theory, is somehow related with the helium flash, since it is observed among stars with mass $M<2$ M_☉ (Kumar et al., 2020). According to Li et al. (2018), Li-rich stars are found on the MS. They argue that this indicates the presence of an unknown efficient process that affects the surface Li abundances before the RGB stage. In addition, Li abundance is a function of various parameters. For instance, Martos et al. (2023) reveal robust anti-correlations between Li abundance and both metallicity and age among solar twins.

Perhaps the most relevant result to mergers between non-compact stars has been recently obtained by Kamiński et al. (2023) on the presence of lithium in three Galactic red nova remnants, which are probably produced by mergers of MS stars. Super-solar lithium abundances they find in these objects ”may suggest that at least some merger products activate mixing mechanisms capable of producing lithium”. V1309 Sco is among these red novae. Its outburst was detected and studied photometrically. It has been established to be caused by the merged stars of a contact binary with the mass of the main companion $\sim 1$ M_☉ (Tylenda et al., 2011) or perhaps somewhat higher, $\sim 1.5$ M_☉. This is now the least massive binary system known to give rise to a red novae (Howitt et al., 2020). This object and studies on its nature were discussed in more detail in Kravtsov et al. (2022).

We obtained new results and complemented them with both a body of observational evidence and theoretical results on binary stars in different environments including GCs. This allowed us to tentatively identify the probable progenitors of G2 stars in the framework of our approach that suggests the binary-mediated merging/collision formation of G2 stars in GCs. These progenitors are high mass-ratio (virtually twin) hard binaries in GCs. They form in any environment, but only in the condition of the high density environment in GCs, and possibly in some other objects, such as ultra-compact dwarf galaxies, the bulge of the Galaxy, etc., these ”seeds” are converted into G2 stars.

The consumption of G1 binaries for building G2 stars means that G1 and G2 sub-populations should be deficient and virtually free of primordial binaries, respectively. This is in agreement with observations that show that the fractions of binaries among G1 sub-populations in GCs are normally an order of magnitude higher than among G2 ones (see Gratton et al., 2019, and references therein).

Primordial (G1) MS stars composing low-mass binaries also undergo an essential transformation due to mass transfer between the components, particularly the accretor. The transferred gas not only increases the accretor’s mass but it can also modify the surface elemental abundances under certain conditions. For example, by using the MESA code, Wei et al. (2020) carried out model studies of surface chemical anomalies of low-mass MS stars due to mass transfer. Their results show that in some low-mass binaries, the accretors can exhibit elemental abundances similar to those of G2 stars, i.e. C and O are in depletion whereas Na and N are in excess (at constant Mg and Al, however), while still remaining on the MS. Note, however, that the donor is considered to be at least as massive as $1$ M_☉ and the final result depends on a few other key parameters including the mass ratio that is typically adopted to be q$=0.5$. When the accretor evolves and is on the RGB, these abundance anomalies can become weaker or disappear entirely. Therefore, given these model results, one can note two useful points. First, the mass-transfer binaries that recently were at the stage of blue stragglers and now are (their accretors) at the RGB, are expected to originally be of systematically lower mass ratio as compared to their counterparts, hard binaries with q$>0.8$ that merged a long ago (G2 stars) and actually are also on the RGB. Second, how many of the actually observed RGB stars in GCs are the evolved blue stragglers? Wei et al. (2021) estimated that their fraction is about 10%. Our estimate (Kravtsov & Calderón, 2021) made for the GC NGC 3201 taking the observed number of blue stragglers in this GC cluster into account is of the same order of magnitude, possibly slightly smaller. However, strictly speaking, this fraction depends on the specific frequency of blue stragglers recently ($\sim 1$ Gyr ago) populated GCs. Normally, the specific frequency of the presently observed blue stragglers is higher in GCs with higher fractions of binary stars (see Milone et al., 2012; Chatterjee et al., 2013, and references therein).

By considering the particular example of NGC 3201, Kravtsov & Calderón (2021) paid attention that the present-day RGB stars in GCs are not uniform in terms of their mass, since not all of them are the progenies of the primordial MS stars. One (minor) fraction are the relatively recently evolved blue stragglers of any nature (with mass typically $M_{\rm BS}>1.1$ M_☉) and another fraction of RGB stars are expected to be the progenies of merger/collision products of the primordial MS stars (latter, in Kravtsov et al. (2022) and in the present paper we argued that the bulk of G2 stars can be such products). By relying on the models of Sills et al. (2009), Kravtsov & Calderón (2021) argued also that such products should achieve the RGB and evolve on it together with the progenies of the primordial stars of (typically) lower mass. In this context, it is worth noting recent results on estimating the masses of stars belonging to the advanced stages of evolution, mainly the RGB, by using asteroseismic observations of the GCs M4 (Howell et al., 2022) and M80 (Howell et al., 2023). Several outliers with masses exceeding $M_{\rm RGB}>1$ M_☉ were detected as candidates evolved blue stragglers. Moreover, an increased dispersion of the derived masses of RGB stars, excluding the outliers, at and below the RGB bump allows to assume a real variation of mass of the order of $\sim 0.05$ M_☉.

The present paper aims at developing further our recently proposed approach (Kravtsov et al., 2022) on the merger/collision nature of G2²²2In the present paper, we use the terms multiplicity, first and second generations (G1 and G2) to follow the definitions adopted in the widely accepted paradigm of multiple stellar populations in GCs, which unambiguously implies the canonical mode of the formation of G2 stars from the gas produced by G1, (very) massive and intermediate-mass stars. Perhaps, G1 and G1_tr (transformed) instead of G1 and G2 (or P1 and P2), respectively, would be more appropriate for our conceptual framework. stars in GCs. The new results reported in the present paper are added with a variety of important both observational evidence and theoretical results obtained so far in various works on this and closely related subjects. Thereby, we further argue a new way of understanding the origin of G2 stars.