On interpolations from SUSY to nonSUSY strings and their properties
Abstract
The interpolation from supersymmetric to nonsupersymmetric heterotic theories is studied, via the ScherkSchwarz compactification of supersymmetric theories to . A general modularinvariant ScherkSchwarz deformation is deduced from the properties of the theories at the endpoints, which significantly extends previously known examples. This wider class of nonsupersymmetric theories opens up new possibilities for model building. The full oneloop cosmological constant of such theories is studied as a function of compactification radius for a number of cases, and the following interpolating configurations are found: two supersymmetric theories related by a duality transformation, with intermediate maximum or minimum at the string scale; a nonsupersymmetric theory interpolating to a supersymmetric theory, with the theory possibly having an AdS minimum; a “metastable” nonsupersymmetric theory interpolating via a theory to a supersymmetric theory.
1.2
IPPP/16/123
Contents
 I Motivation for studying interpolating models
 II The cosmological constant and generalized ScherkSchwarz construction
 III On SUSY Restoration
 IV Surveying the interpolation landscape
 V Conclusions
 A Notation and conventions for partition functions
 B Conventions and spectrum of the fermionic string
I Motivation for studying interpolating models
An important question in string phenomenology is how and when supersymmetry (SUSY) is broken. A great deal of effort has been devoted to frameworks in which it is broken nonperturbatively in the supersymmetric effective field theory. Much less effort has been devoted to string theories that are nonsupersymmetric by construction.
On the face of it, the trade off for the second option, is that nonsupersymmetric string models do not have the stability properties of supersymmetric ones. However it can be argued that as long as the SUSY breaking is spontaneous and parametrically smaller than the string scale, the associated instability is under perturbative control Abel:2015oxa (). There is then no genuine moral, or even practical, advantage to the former more traditional option, since nature is not supersymmetric. Sooner or later, either route to the Standard Model (SM) will lead to runaway potentials for moduli that need to be stabilised. Indeed spontaneous breaking at the string level may even confer advantages in this respect, as discussed in ref.Abel:2016hgy ().
Parametric control over SUSY breaking requires a generic method for passing from a nonsuperymmetric theory to a supersymmetric counterpart, under certain limiting conditions. The method that was studied in ref.Abel:2015oxa () is interpolation via compactification to lower dimensions, with SUSY broken by the ScherkSchwarz mechanism scherkschwarz (). The two great advantages of interpolating models are that their compactification volumes can be tuned to make the cosmological constant arbitrarily small, and that some of them exhibit enhanced stability due to a oneloop cosmological constant that is exponentially suppressed with respect to the generic SUSY breaking scale Abel:2015oxa (). They can be viewed as natural and phenomenologically interesting extensions of the original observation in refs.Itoyama:1986ei (); Itoyama:1987rc () that the tachyonfree nonsupersymmetric model interpolates to the heterotic model, via a ScherkSchwarz compactification to .
The general properties under interpolation of theories broken by the ScherkSchwarz mechanism are not known. For example, what determines if the zero radius endpoint theory is supersymmetric? This paper focusses on the properties of dimensional () theories that interpolate between stable, supersymmetric tachyonfree models. Three main results are presented.

First, we derive and study the general form of the endpoint theories, and show that their modular invariance properties derive directly from the ScherkSchwarz deformation. This enables us to generalise the construction of modular invariant ScherkSchwarz deformed theories by beginning with the endpoint theory.

Second, we determine a simple criterion for whether a SUSY theory, broken by ScherkSchwarz, will interpolate to a SUSY or a nonSUSY one at zero radius: the zero radius theory is nonsupersymmetric, if and only if the ScherkSchwarz acts on the gauge group as well as the spacetime side.

Third, we undertake a preliminary survey (in the sense that the models we study only have orthogonal gauge groups) of some representative models that confirm these two properties, by examining their potentials and spectra.
The general framework for the interpolations are as shown in Figure 1. Beginning with a supersymmetric theory generically referred to as , the theory is compactified to a nonsupersymmetric theory by adapting the Coordinate Dependent Compactification (CDC) technique first presented in refs.Kounnas:1989dk (); Ferrara:1987es (); Ferrara:1987qp (); Ferrara:1988jx (). This is the string version of the ScherkSchwarz mechanism, which spontaneously breaks SUSY in the theory with a gravitino mass of where is the largest radius carrying a ScherkSchwarz twist. (We will use “CDC” and “ScherkSchwarz” interchangeably.) As usual it is the gravitino mass that is the order parameter for SUSY breaking: it can be continuously dialled to zero at large radius where SUSY is restored and regained.
One of the main properties that will be addressed is the nature of the theory as the radius of compactification is taken to zero. This depends upon the precise details of the ScherkSchwarz compactification, and indeed we will find that the presence or otherwise of SUSY at zero radius depend on the choice of basis vectors and structure constants defining the model. It is possible that the theory interpolates to either a supersymmetric or a nonsupersymmetric model ( or respectively). Models of the latter kind correspond to a theory in which SUSY is broken by discrete torsion Abel:2015oxa ().
We begin in §II.1 by reviewing the basic formalism for interpolation. Section II.2 then presents the construction of nonsupersymmetric models as compactifications of supersymmetric ones. The modification of the massless spectra in the decompactification and limits (with the latter corresponding to the decompactification limit of a dual theory) is analysed, in order to determine the nature of the theories at the small and large radii endpoints. Section II.3 discusses the technique for rendering the cosmological constant in an interpolating form, allowing it to be calculated across a regime of small and large radii. The modification of the projection conditions and massless spectrum by the choice of basis vectors and structure constants is made explicit, and based on these observations, in particular how the CDC correlates with modified GSO projections in the endpoint theories, §II.4 then derives the general form of deformation within this framework, extending previous constructions. This more general formulation may prove to be useful for future model building.
The conditions under which SUSY is preserved or broken at the endpoints of the interpolation are discussed in §III. Particular focus is given to the constraints on the appearance of light gravitino winding modes in the zero radius limit. It is found that models in which the CDC acts only on the spacetime side, are inevitably supersymmetric at zero radius, while models within which the CDC vector is nontrivial on the gauge side as well yield a nonsupersymmetric model in the same limit. This analysis paves the way for a presentation in §IV of explicit interpolations (in terms of their cosmological constants) in particular models that display various different behaviours: namely we find examples of interpolation between two supersymmetric theories via theories with negative or positive cosmological constant; interpolation between a nonsupersymmetric theory and a supersymmetric one, with or without an intermediate AdS minima; we also find examples of “metastable” nonsupersymmetric theories (by which we mean theories that have a positive cosmological constant with an energy barrier) that can decay to supersymmetric ones.
As mentioned, this paper follows on from a reasonably large body of work on nonsupersymmetric strings that is nonetheless much smaller than the work on supersymmetric theories. Following on from the original studies of the tendimensional heterotic string SOsixteen (), there were further studies of the oneloop cosmological constants Rohm (); nonSUSYgauge (); Itoyama:1986ei (); Itoyama:1987rc (); Moore (); Dienes:1990ij (); KutasovSeiberg (); heretic (); missusy (); supertraces (); Kachru:1998hd (); KachSilvothers (); Shiu:1998he (); Iengo:1999sm (); DhokerPhong (); Faraggi:2009xy (), their finiteness properties missusy (); supertraces (); Angelantonj:2010ic (), their relations to strong/weak coupling duality symmetries Bergman:1997rf (); julie1 (); julie2 (); Faraggi:2007tj (), and string landscape ideas Dienes:2006ut (); Dienes:2012dc (). The relationship to finite temperature strings was explored in refs. finitetemp (); AtickWitten (); wasKounnasRostand (); Kounnas:1989dk (); earlystringpapersfiniteT ()). Further development of the ScherkSchwarz mechanism in the string context was made in refs.Kiritsis:1997ca (); Dudas:2000ff (); Scrucca:2001ni (); Borunda:2002ra (); Angelantonj:2006ut (). Progress towards phenomenology within this class has been made in refs. Lust:1986kj (); Lerche:1986ae (); Lerche:1986cx (); nonSUSYgauge (); Chamseddine:1988ck (); Font:2002pq (); Faraggi:2007tj (); Blaszczyk:2014qoa (); Angelantonj:2014dia (); Blaszczyk:2015zta (); Nibbelink:2016lzi (). Related aspects concerning solutions to the largevolume “decompactification problem” were discussed in refs.Faraggi:2014eoa (); Kounnas:2015yrc (); Partouche:2016xqu (); Kounnas:2016gmz (); Abel:2016hgy (). Nonsupersymmetric string models have also been explored in a wide variety of other configurations othernonsusy (); Sagnotti:1995ga (); Sagnotti:1996qj (); Angelantonj:1998gj (); Blumenhagen:1999ns (); Sugimoto:1999tx (); Aldazabal:1999tw (); Angelantonj:1999xc (); Forger:1999ev (); Moriyama:2001ge (); Angelantonj:2003hr (); Angelantonj:2004yt (); Dudas:2004vi (); GatoRivera:2007yi (), including studies of the relations between scales in various schemes Antoniadis:1988jn (); Antoniadis:1990ew (); Antoniadis:1992fh (); Antoniadis:1996hk (); Benakli:1998pw (); Bachas:1999es (); Dudas:2000bn (). Some aspects of this study are particularly relevant to the recent work in refs.Florakis:2016aoi ().
Note that here we will not elaborate on the properties of the nonsupersymmetric theory at radii of order the string length. As we will see, and as found in ref.Abel:2015oxa (), often there is a minimum in the cosmological constant at this point which suggests some kind of enhancement of symmetry at a special radius. (Indeed often it is possible to identify gauge boson winding modes that become massless at the minimum.) There is therefore the possibility of establishing connections to yet more nonsupersymmetric theories. Conversely one can ask if every nonsupersymmetric tachyonfree theory can be interpolated to a supersymmetric higher dimensional theory. We comment on this and other prospects in the Conclusions in §V.
Ii The cosmological constant and generalized ScherkSchwarz construction
ii.1 Overview
In this section, we revisit the calculation of the cosmological constant in the ScherkSchwarzed theories, and in particular derive a formulation for the partition function of interpolating models, that is useful for the later analysis. The discussion is a natural generalisation of the “compactificationonacircle” treatment of ref.Abel:2015oxa (), and as we shall see it ultimately leads to an improved and more general construction for this class of theory.
Let us begin by briefly summarising the implementation of the ScherkSchwarz mechanism described in that work. As already mentioned, this is incorporated using a Coordinate Dependent Compactification (CDC) Kounnas:1989dk () of an initially supersymmetric theory, namely the model. For our purposes it is useful to define it in the fermionic formulation, although any construction method would be applicable. In this formulation, the initial theory is defined by assigning boundary conditions to worldsheet fermions. If they are real, this is encapsulated in a set of 28dimensional basis vectors, , containing periodic or antiperiodic phases. The sectors of the theory are given by the set of where so that . We follow the usual the convention that denotes the sum over spin structures on the cycle. The spectrum of the theory at generic radius in any sector is determined by imposing the GSO projections governed by the vectors and a set of structure constants , according to the KLST set of rules in refs.Kawai:1986ah (); Kawai:1986va (); Kawai:1986vd (); Kawai:1987ew () (and equivalently ref.Antoniadis:1986rn ()), which are summarised in Appendix, B.
The model is then further compactified down to on a orbifold. In the absence of any CDC the result would simply be an model resulting from an overall compactification. The in question corresponds to the theory in the fermionic construction in our examples. In theories of the type discussed in Abel:2015oxa (), in which the orbifold twist preserves SUSY, the twisted sectors have a supersymmetric spectrum, and therefore do not contribute to the cosmological constant, and thus the nature of the orbifold is unimportant. The CDC is implemented by introducing a deformation, described by another vector , of shifts in the charge lattice that depend on the radii of the ; this will be shown explicitly below. Under the CDC, the Virasoro generators of the theory are modified, yielding an extra effective projection condition, (in addition to the GSO projections associated with the from which the initial is constructed), governed by , on the states constituting the massless spectrum of the theory. The remaining massless states are then characterized by their charges under the symmetry associated with . To qualify as a ScherkSchwarz mechanism, this symmetry has to include some component of the symmetry in order to distinguish bosons from fermions, thereby projecting out the gravitinos, and breaking spacetime SUSY.
The effect of the CDC of course disappears in the strict limit where the KaluzaKlein (KK) spectrum becomes continuous, and the endpoint model is recovered. On the other hand as we shall see the CDC turns into another GSO projection vector in the limit, where states either remain massless or become infinitely massive. Upon dualising,
(1) 
the model becomes the noncompact theory , whose properties depend precisely on the form of .
The theories at the two endpoints can contain a different number of states and charges. Because can overlap the gauge degrees of freedom, will generically have a gauge symmetry that differs from that of , and possibly no SUSY. As we will see the two are in fact linked: if is supersymmetric then the gauge group is the same as that of , if it is not, then the gauge group is different.
ii.2 CDCModified Virasoro Operators
Let us now elaborate on the above description. The conventions for the fermionic construction are as in refs.Kawai:1986ah (); Kawai:1986va (); Kawai:1986vd (); Kawai:1987ew () and for the CDC are as outlined in ref.Abel:2015oxa (), and summarised in Appendix B. That is the unmodified Virasoro operators are defined as
(2) 
where, in terms of the winding and KK numbers, and respectively, the left and rightmoving momenta for a theory compactified on two circles of radii take the unshifted form
(3) 
Ultimately we wish to derive the largest possible class of deformations to the Virasoro operators that is compatible with modular invariance. This will turn out to be more general than those considered in refs.Ferrara:1988jx (); Kounnas:1989dk (). In order to achieve this, we will now display the most general modification possible of the Virasoro operators under the ScherkSchwarz action, along with a free parameter , which will ultimately be fixed by imposing modular invariance:
(4) 
where the other oscillator contributions can be deduced from 57, and where are the vectors of Cartan gauge and charges, defined by . As promised, the parameter will now be determined by modular invariance. The partition function of the modified theory is then expressed in terms of (where as usual the real and imaginary parts of are defined to be ):
(5) 
Modular invariance requires . Given that the original supersymmetric theory is modular invariant (i.e. ) this can be used to determine a consistent as follows:
(6) 
where the dot products are Lorentzian. Thus a KK shift of
(7) 
is sufficient to maintain modular invariance in the deformed theory. This matches the result of ref. Kounnas:1989dk (). The vector then lifts the masses of states according to their charges under the linear combination . Restricting the discussion to halfinteger massshifts imposes the constraint mod(2). Later on the partition function will be reorganised into sums over different values of (as we restrict the study to phases in all examples, fractions of at most can arise in the GSO projections via odd numbers of overlapping ’s). So far these deformations are precisely those of refs.Kounnas:1989dk (); Ferrara:1987es (); Ferrara:1987qp (); Ferrara:1988jx (): once we consider the interpolation to the theories, it will become clear how they can be made general.
Note that levelmatching is preserved by the CDC, but the mass spectrum is modified rather than the number of degrees of freedom contained within the theory, as required for a spontaneous breaking of SUSY Kounnas:1989dk (); Ferrara:1987es (); Ferrara:1987qp (); Ferrara:1988jx (). It is clear from eq.(II.2) that for zero winding modes (), states for which become massive under the action of the CDC. Conversely all the zero winding states in the NSNS sector remain unshifted by the CDC since they are chargeless. As described in ref.Abel:2015oxa () there may or may not be massless gravitinos depending on whether the effective projection is aligned with the other projections: this is in turn dependent on the choice of structure constant, so that ultimately the breaking of SUSY is associated with breaking by discrete torsion.
ii.3 Details of Cosmological Constant Calculation
To evaluate the cosmological constant, at given radii , one must integrate each term (weighted by its coefficient ) in the total 1loop partition function over the fundamental domain of the modular group:
(8) 
where is the number of uncompactified spacetime dimensions (equal to 4 at all intermediate radii between the small and large radius endpoint theories, along which the cosmological constant will be evaluated), and is the reduced string scale. Henceforth is set to 1; it can be reinserted by dimensional analysis at the end of the calculation if desired. The integral splits into upper () and lower regions of the fundamental domain. Only terms for which can receive contributions from both regions, with the integral yielding zero in the upper region when , enforcing level matching in the infrared (but allowing contributions from unphysical protograviton modes in the ultraviolet as described in ref.Abel:2015oxa ()).
At general radius the evaluation of the cosmological constant is complicated immensely by the fact that vary with . In order to make the evaluation tractable, the total partition function, , has to be rearranged into separate bosonic and fermionic factors as follows. It is convenient to define and . Twisted sectors do not need to be considered in this implementation as, being supersymmetric, they do not contribute to the cosmological constant. In other words, the cosmological constant calculated without the orbifolding, is the same up to a factor of two, as the actual cosmological constant, as explained in detail in Kounnas:1989dk (); Ferrara:1987es (); Ferrara:1987qp (); Ferrara:1988jx (); Abel:2015oxa (). However, we will make further comments on twisted sectors later when we come to generalise the construction. We have
(9) 
where the Poissonresummed partition function for the compactified complex boson is given by (see Appendix A)
(10) 
and the theta function products, each of which has characteristics defined by the sectors , with their respective CDC shifts, are
(11) 
where the conventions can be found in Appendix A.
In the above, the coefficients of the partition function are given by
(12) 
where are the coefficients of the original theory before CDC, expressed in terms of the structure constants , and spinstatistic , as in the original notation and Appendix B, namely
(13) 
It is convenient to use the resummed version of this expression; certainly for the expansion this is the preferred method as it makes modular invariance explicit. This removes the prefactor and adds a factor of . The bosonic factor in the partition function depend upon the radii of compactification, the winding and resummed KK numbers and the CDC induced shift in the KK levels, , as follows:
(14) 
The effective shift in the KK number, given by the requisite , arises from the choice of , which gives an overall phase in the partition function; as we shall see this shift in the KK number ultimately amounts to introducing a new vector in the noncompact dual theory at zero radius, combined with structure constants , . Note that this means in the 4D spectrum one may find states with 1/4charges , that since they have , become infinitely massive in the zero radius limit.
In order to reorder the sum to do it efficiently, a projection in the on is now introduced to select possible values of . Following the notation that represents the sum over spin structures, the parameter for this projection over the vector will be called . Thus overall, using the results in Appendix A, one can write,
(15) 
where
(16) 
Note that the phases in are precisely what is needed to cancel the contribution coming from the theta functions in , so that overall the spectrum is merely shifted, with the GSO projections remaining independent of .
The bosonic contribution to the total partition function is independent of the fermionic sectors within the theory so appears as a prefactor to the sector sum for any given . Conversely, the fermionic partition function is composed of terms that depend upon the boundary conditions of the fermions within the sectors each of which is independent of the compactification radii. The advantage of this reordering is that one can therefore collect 16 representative factors, ,
(17) 
which are independent of the radii, and 16 respective factors (), which being independent of the internal degrees of freedom, depend only on the compactification,
(18) 
The latter are radius dependent interpolating functions, analogous to the functions in the simple circular case studied in ref.Abel:2015oxa (). We refer to the terms as ’ factors’, since they involve only the internal degrees of freedom of the theory, and thus can be computed for all radii at the beginning of the calculation. The total partition function is then compiled by summing over the 16 sectors as
(19) 
To summarise, via the procedure of reordering the original sum 9, a projection on to different consistent values has been performed, such that a sum over can now be taken.
ii.4 The zero radius theory and a more general formulation of ScherkSchwarz
An interesting aspect of the above approach is that in the small radius limit, that part of the spectrum with mod(1) decouples and can be discarded, leaving the partition function of the noncompact theory at . Indeed, Poisson resumming on and gives
(20) 
where the ellipsis indicate terms that are further exponentially suppressed. Thus the total untwisted partition function in the small radius limit can be expressed as
(21) 
Note that is simply the expected volume factor of the partition function in the dual theory. In conjunction with the fermionic component of the partition function, this then reproduces a model with an additional basis vector , appearing in the sector definitions as , and with eq.(7) providing a new GSO projection, namely mod (1). (The mod (1) comes courtesy of the sum over .)
Upon inspection therefore, we are finding that eq.(7) is actually the GSO projection of an additional vector in the noncompact theory. Beginning with the choice of , one can infer that the theory at zero radius for the examples we have been considering has structure constants and , consistent with the modular invariance rules of KLST in refs.Kawai:1986ah (); Kawai:1986va (); Kawai:1986vd (); Kawai:1987ew (). In fact identifying sectors as with the sum over the spin structures on the cycle as mod(2), the entire partition function at zero radius is that of the theory with the appropriate corresponding GSO phases,
(22) 
Reversing the line of reasoning above, leads us finally to a generalisation of the construction of interpolating models based on the modular invariance of their endpoint theories:

First, define a theory in terms of a set of vectors , and any additional vector that obeys the modular invariance rules of ref.Kawai:1986ah (); Kawai:1986va (); Kawai:1986vd (); Kawai:1987ew (), together with a set of consistent structure constants and . (The are then fixed by the modular invariance rules in the usual way.)

In theories that have an additional orbifold action on compactification to , is still constrained by the need to preserve mutually consistent GSO projections, with the condition (as in refs.Ferrara:1988jx (); Kounnas:1989dk () and discussed in ref.Abel:2015oxa ()).
The last statment, namely that one may simply treat the ScherkSchwarz action as another basis vector, leading to considerable generalisations, is one of the main results of the paper. In order to prove it, one may first Poissonresum back to the original expression but retaining , so that entire partition function is
(24) 
Note that the sum over provides a projection that equates mod(1). Using the modular transformations for theta functions detailed in Appendix A, it is then straightforward to show that the partition function is invariant under provided that
(25) 
and invariant under provided that
(26) 
This overall set of conditions is precisely that of KLST Kawai:1986ah (); Kawai:1986va (); Kawai:1986vd (); Kawai:1987ew () with the original theory enlarged to include the vector .
Note that these rules are significantly more general than those of refs.Kounnas:1989dk (); Ferrara:1987es (); Ferrara:1987qp (); Ferrara:1988jx (), in which the choice
(27) 
corresponds to taking and , in 22. Now for example the CDC vectors are no longer restricted to obey mod(1), and
moreover the KK shifts have additional sector dependence if . We should add that, as well as being a generalisation, these rules simplify the construction of viable phenomenological models, because the condition can be implemented independently, with consistency then guaranteed with respect to
all the other vectors
Iii On SUSY Restoration
iii.1 Is the theory at small radius supersymmetric?
Let us now move on to the conditions under which the endpoint theories exhibit SUSY. We will always consider models in which the theory at infinite radius is supersymmetric (as would be evidenced by the vanishing of the cosmological constant there) but we would like to determine whether or not SUSY is restored at zero radius as well. In this section we develop arguments to address this question based on the existence or otherwise of massless gravitinos as .
As usual the pure NeveuSchwarz (NSNS) sector, gives rise to the gravity multiplet, (the graviton), (the dilaton) and (the two index antisymmetric tensor), from the states in the notation of ref.Abel:2015oxa (). These states are chargeless under and no projection on them can occur, since the CDC vector is always zero in the spacetime dimensions . Given the inevitable presence of the graviton, the SUSY properties of the theory are then dictated by the presence or absence of the RNS gravitinos, namely
Their ScherkSchwarz projections are determined purely by the ScherkSchwarz action on the rightmoving degrees of freedom
The spectrum is found from the expressions for the modified Virasoro operators in eq.(II.2). For the nonwinding gravitinos, the shifted KK momentum becomes virtually continuous in the limit and the full gravitino state is inevitably recovered there. The scale at which SUSY is spontaneously broken by the CDC is set by the gravitino mass . As the compactification is turned on, the SUSY of the theory is broken, and then towards the end of the interpolation, new gravitinos may or may not appear in the massless spectrum, perhaps heralding the restoration of SUSY at small radius as well.
To see if they do, consider how the CDC modifies the theories that sit at the endpoints of the interpolation. We denote by the charge of the lightest gravitino state at large radius. SUSY is exact even in the presence of , with the state being exactly massless, if both the first and second terms in the modified Virasoro operators of eq.(II.2), namely
(28) 
and
(29) 
vanish. (For convenience we continue for this discussion to use the original more restrictive rules of refs.Kounnas:1989dk (); Ferrara:1987es (); Ferrara:1987qp (); Ferrara:1988jx (); it would be trivial to extend the discussion to the more general rules of eq.(23).) With , the first term receives no extra contribution due to the CDC. Furthermore, there is no winding contribution to the second term. Therefore gravitinos that have remain massless and indicate the presence of exact SUSY. Conversely, if the only remaining gravitinos have
(30) 
their mass is and SUSY is spontaneously broken.
Without loss of generality, one can consider SUSY breaking to amount to a conflict between and a single basis vector, denoted by . That is, constrains the gravitinos, while the remaining cannot project them out of the theory. In order for the above light (but not massless) gravitino to be the one that is left unprojected, the projections due to and must disagree, that is the massive state is retained by while the massless state is projected out. Again without loss of generality, it is always possible to choose so that the conditions are aligned; that is . These modes are preserved (and have a mass ) while projects the massless modes out of the theory entirely.
Now consider the zero radius end of the interpolation, and denote the new wouldbe massless gravitino state by . Although a different state, it can be related to the infinite radius gravitino by a shift in the charge vector, induced by a potentially nonzero winding number;
(31) 
As vanish, the spectrum associated with the winding modes becomes continuous, while the KK states become extremely heavy. As described in the previous section, the requirement that the KK term in eq.(29) vanishes forms an effective projection that constrains the light states at zero radius, selecting the modes for which
(32) 
where we will assume that .
It is clear from the relation between and in eq.(31) that the projection due to the CDC vector remains unchanged for any gravitino state there, since ; that is
(33) 
This equation together with eqs.(32) and (30), imply that any gravitino of the spontaneously broken theory that becomes light at small radius must be an oddwinding mode. Under the shift in given by eq.(31), the projection constraining the gravitinos is
(34)  
For the effective projection in eq.(32) to agree with the modified GSO condition in eq.(34) for , we then require that
(35) 
Eq.(35) is a necessary condition for a model with SUSY spontaneously broken by the ScherkSchwarz mechanism to have massless gravitino states in both the infinite and zero radius limits.
SUSY restoration when the CDC vector has zero leftmoving entries
Let us see what it implies in a specific theory. Consider the basis vector set , together with a CDC vector that is empty in its leftmoving elements, the standard set up outlined in Abel:2015oxa (), in which the vectors project down to SUSY with orthogonal gauge groups:
(36) 
A suitable and consistent set of structure constants is
Gravitinos are found in the sector, with vacuum energies . The charge operator for the nonwinding gravitinos in the initial (infinite radius) theory takes the same form as the sector vector itself. They have charges determined by that give the required mod (1) for spontaneous SUSY breaking: the positive helicity states with this choice of structure constants are
(37) 
where the signs on the fermions are codependent. It is clear from the vector overlap between and that the latter is playing the role of that constrains the gravitini states. (The structure constants have been chosen such that yields identical constraints.) Whether or not any of the winding modes of the gravitinos are light at zero radius depends upon them satisfying the modified GSO projection condition of eq.(34):
(38) 
As we saw the two projections agree for the oddwinding modes of the states since , and under the CDC, the charge vector for the small radius gravitino is
(39) 
Note that nonzero rightmoving charges of the small radius gravitino are on the and worldsheet degrees of freedom, and they no longer overlap the SUSY charges of the large radius theory.
The appearance of gravitino states in the light spectrum in the zero radius limit of this theory reflects a general conclusion. If the leftmoving elements of the CDC vector vanish, eq.(35) is automatically satisfied. Any theory with a CDC vector acting purely on the spacetime side becomes supersymmetric at zero radius since the projection always preserves the oddwinding modes of the gravitinos. The nonsupersymmetric theory at generic radius is therefore an interpolation between two supersymmetric theories quite generally in these cases, which sit at the zero and infinite radius endpoints. The supersymmetric nature of the zero radius theory will later be verified by the vanishing of the cosmological constant in the limit (Figure 2), as presented in the following section. Note that the necessary cancellation between thousands of terms is highly nontrivial.
Example of a CDC vector with nonzero leftmoving entries
Consider instead a theory composed of the same basis vector set as in eq.(III.1.1), but now with a CDC vector containing nonzero leftmoving entries: for example
(40) 
Under the CDC, and for convenience of presentation dropping the signs, the charge vector for the oddwinding gravitino modes is modified to
(41) 
As in the previous example the vector contains the same number of nonzero rightmoving entries, but lying in different columns, so there is no contribution from eq.(28) to the mass squared on the spacetime side. However the nonzero leftmoving elements now result in a nonzero contribution. Under the shift,
(42) 
any nonzero shift in will inevitably produce massive gravitinos since in the RNS sector the charges of massless states must be zero mod (1) on the leftmoving side.
We conclude that SUSY is restored at small as well as large radius if and only if the ScherkSchwarz mechanism does not act on the gaugeside. Conversely if SUSY is broken at zero radius then so is the gauge symmetry.
iii.2 Formula for ?
The nett bosefermi number appears as the constant term in the parition function . Thus, the dominant terms in the one loop contribution to the cosmological constant are proportional to for the massless states Abel:2015oxa (), so nonsupersymmetric models with an equal number of massless bosonic and fermionic states have an exponentially suppressed oneloop cosmological constant, and hence exhibit an increased degree of stability. Unfortunately it seems to be necessary to determine the full massless spectrum in order to deduce whether or not . There appears to be no principle, or algebraically feasible generic procedure, for choosing the basis vectors , the CDC vector , and the structure constants , that ensures that .
Iv Surveying the interpolation landscape
We now turn to a survey of the different possible interpolations, in order to verify the rules derived in the previous sections, in particular those that govern the supersymmetry properties of the models. We should remark that in order to make the exercise computationally feasible, we will only use 1/2 phases so that the theories contain only large orthogonal gauge groups. As such, we are not here attempting to construct the SM, and the massless spectrum for each example will not be presented. (They can easily be determined using the rules in Appendix B). Rather, studying the relationship between the cosmological constant and the radii of compactification exemplifies interpolation patterns between different types of model. Following the procedure outlined in Section II.3, the total partition function, , truncated at an order in the expansion, which is computationally manageable while displaying the qualitative behaviour, is input in to the integral in 8, for a range of compactification radii between either ends of the interpolation range.
iv.1 Interpolation Between Two Supersymmetric Theories
Nb>Nf
Consider a theory containing , and as in the above basis vector set in eqs.(III.1.1), a modified , an additional vector , and a CDC vector that acts only on the spacetime side:
(43) 
A suitable and consistent set of structure constants is
This model can be investigated using the general method presented in the previous section. plays the role of , while respects its projections on the gravitinos. As discussed the interpolation is between two supersymmetric endpoints at both small and large radius. The cosmological constant takes a nonzero negative value with a minimum at intermediate values, and returns to zero at the two extremes, displayed in Figure 2.
Nb<Nf
A theory in which can be generated by a performing an alternative modification to the vectors :
(44) 
with the following structure constants:
Similarly to the model with a exclusively nontrivial rightmoving CDC vector, this model interpolates between two supersymmetric endpoints at both small and large radius, with the cosmological constant now taking a nonzero positive value at intermediate radii, displayed in Figure 3, corresponding to unstable runaway to decompactification at either end of the interpolation.
iv.2 Interpolation from a Nonsupersymmetric to a Supersymmetric Theory
Nb=Nf
A theory with BoseFermi degeneracy can be achieved with a theory comprised of the basis vector set in eq.(III.1.1), plus a basis vector