Student or educator? Sign up with your school email and get 6 months of Pro free.
CoChat
Sign Up
Cited by 14

The DOI matches its Crossref record; 9 of the 9 references it cites were found in a registry or an index.

De Sitter decays to infinity

Draper, Patrick, Garcia, Isabel Garcia, Lillard, Benjamin·2021·Journal of High Energy Physics
DOI 10.1007/jhep12(2021)154
Open this paper in CoChat — free account

Abstract

Bubbles of nothing are a class of vacuum decay processes present in some theories with compactified extra dimensions. We investigate the existence and properties of bubbles of nothing in models where the scalar pseudomoduli controlling the size of the extra dimensions are stabilized at positive vacuum energy, which is a necessary feature of any realistic model. We map the construction of bubbles of nothing to a four-dimensional Coleman-De Luccia problem and establish necessary conditions on the asymptotic behavior of the scalar potential for the existence of suitable solutions. We perform detailed analyses in the context of five-dimensional theories with metastable dS 4× S1 vacua, using analytic approximations and numerical methods to calculate the decay rate. We find that bubbles of nothing sometimes exist in potentials with no ordinary Coleman-De Luccia decay process, and that in the examples we study, when both processes exist, the bubble of nothing decay rate is typically faster. Our methods can be generalized to other stabilizing potentials and internal manifolds.

Overview

The claims and statistics of this paper haven’t been checked yet.

Run the check — free, no account needed. It reads the open-access text and checks the sources it cites.

A few free checks a day · papers already verified open instantly · results are public

Integrity signals

Registry

Crossref · 10.1007/jhep12(2021)154

Cites

9 of 9 references verified0 citation errors · 0 not checkable

Statistics

Figures

Image 1
CC-BY · From the PDF
Figure 3 Diagram R5 Figure 11: Just L ( ) 5 Figure 2 . Left: diagram showing the geometry of the KK false vacuum ('vacuum') and BON ('instanton') solutions. The r direction lies along the symmetry axis, with the periodic y coordinate along the azimuth. In the false vacuum, φ ≡ 0 , and the KK radius is independent of r . For Witten's bubble, the KK radius approaches zero near r ≳ R 5 , whereas far away from the bubble wall the geometry asymptotically approaches that of the false vacuum. Right: after dimensional reduction, the scalar modulus φ describes the proper length of the KK circle, L . As a function of the CDL coordinate, defined in eq. (2.20), L vanishes at ξ = 0 , corresponding to the location of bubble wall, whereas L ≃ 2 πR 5 in the asymptotic region ξ ≫ R 5 .
Figure 3 Diagram R5 Figure 11: Just L ( ) 5 Figure 2 . Left: diagram showing the geometry of the KK false vacuum ('vacuum') and BON ('instanton') solutions. The r direction lies along the symmetry axis, with the periodic y coordinate along the azimuth. In the false vacuum, φ ≡ 0 , and the KK radius is independent of r . For Witten's bubble, the KK radius approaches zero near r ≳ R 5 , whereas far away from the bubble wall the geometry asymptotically approaches that of the false vacuum. Right: after dimensional reduction, the scalar modulus φ describes the proper length of the KK circle, L . As a function of the CDL coordinate, defined in eq. (2.20), L vanishes at ξ = 0 , corresponding to the location of bubble wall, whereas L ≃ 2 πR 5 in the asymptotic region ξ ≫ R 5 .CC-BY · From the PDF
Figure 6 Cartoon 3 Figure 3 . The five-dimensional Euclidean Schwarzschild gravitational instanton, or Witten's BON, expressed in terms of the degrees of freedom φ bon ( ξ ) ( left ) and ρ bon ( ξ ) ( right ) of the corresponding CDL problem. The behavior of the solutions in the near-horizon ( ξ ≪ R 5 ) and asymptotic ( ξ ≫ R 5 ) regimes is indicated in the figure, following eq. (2.21) and eq. (2.22), respectively.
Figure 6 Cartoon 3 Figure 3 . The five-dimensional Euclidean Schwarzschild gravitational instanton, or Witten's BON, expressed in terms of the degrees of freedom φ bon ( ξ ) ( left ) and ρ bon ( ξ ) ( right ) of the corresponding CDL problem. The behavior of the solutions in the near-horizon ( ξ ≪ R 5 ) and asymptotic ( ξ ≫ R 5 ) regimes is indicated in the figure, following eq. (2.21) and eq. (2.22), respectively.CC-BY · From the PDF
Figure 6 Cartoon 3 Figure 4 . A diagram comparing the BON and CDL boundary conditions. The BON initial conditions φ (0) → -∞ , φ ′ → + ∞ ensure that φ ( ξ ) quickly approaches the false vacuum. Its approach to φ ( ξ ) → φ fv is determined by the details of the potential, which is approximately quadratic in the neighborhood of φ ≈ φ fv . This direct approach to φ fv is indicated by the straight blue line in the figure. The CDL solution, on the other hand, begins at finite φ (0) = φ CDL with φ ′ (0) = 0 . It subsequently 'rolls' in the inverted potential, as indicated by the dashed red line, until it approaches φ fv . In the dashed blue line we show a second BON example, one in which the potential U ( φ → -∞ ) diverges (with -U ( φ ) shown in dark gray). The φ ′ (0) → ∞ BON initial conditions can compensate for the divergence in U ( φ ) , so that there is a BON solution even if there is no corresponding CDL solution for that potential.
Figure 6 Cartoon 3 Figure 4 . A diagram comparing the BON and CDL boundary conditions. The BON initial conditions φ (0) → -∞ , φ ′ → + ∞ ensure that φ ( ξ ) quickly approaches the false vacuum. Its approach to φ ( ξ ) → φ fv is determined by the details of the potential, which is approximately quadratic in the neighborhood of φ ≈ φ fv . This direct approach to φ fv is indicated by the straight blue line in the figure. The CDL solution, on the other hand, begins at finite φ (0) = φ CDL with φ ′ (0) = 0 . It subsequently 'rolls' in the inverted potential, as indicated by the dashed red line, until it approaches φ fv . In the dashed blue line we show a second BON example, one in which the potential U ( φ → -∞ ) diverges (with -U ( φ ) shown in dark gray). The φ ′ (0) → ∞ BON initial conditions can compensate for the divergence in U ( φ ) , so that there is a BON solution even if there is no corresponding CDL solution for that potential.CC-BY · From the PDF
antipodal points of S 3 Figure 4: Diagram R5 2 1.5 Figure 9: Piecewise toy potential U ( ), together with more realistic examples 4 Figure 5 . Left: the piecewise potential U toy ( φ ) from eq. (3.17), with φ 1 = -0 . 2 M p and U fv = 0 . 2 U 0 . Right: the quantity φ ⋆ = -m 2 R 2 5 2 √ 3 2 M p indicates the point where the potential U ( φ ) begins to have a noticeable effect on the equation of motion for φ (see the discussion around eq. (3.45)). For φ ≪ φ ⋆ , φ ( ξ ) is well approximated by the Witten BON solution, even if the potential U ( φ ) is large. This feature greatly enhances the utility of the piecewise quadratic toy model. All three of the 'realistic' smooth potentials will have similar solutions for φ ( ξ ) and ρ ( ξ ) , despite the significant differences in their asymptotic φ →-∞ limits, as long as mR 5 ≪ 1 is small enough that U ( | φ | ≤ | φ ⋆ | ) remains approximately quadratic.
antipodal points of S 3 Figure 4: Diagram R5 2 1.5 Figure 9: Piecewise toy potential U ( ), together with more realistic examples 4 Figure 5 . Left: the piecewise potential U toy ( φ ) from eq. (3.17), with φ 1 = -0 . 2 M p and U fv = 0 . 2 U 0 . Right: the quantity φ ⋆ = -m 2 R 2 5 2 √ 3 2 M p indicates the point where the potential U ( φ ) begins to have a noticeable effect on the equation of motion for φ (see the discussion around eq. (3.45)). For φ ≪ φ ⋆ , φ ( ξ ) is well approximated by the Witten BON solution, even if the potential U ( φ ) is large. This feature greatly enhances the utility of the piecewise quadratic toy model. All three of the 'realistic' smooth potentials will have similar solutions for φ ( ξ ) and ρ ( ξ ) , despite the significant differences in their asymptotic φ →-∞ limits, as long as mR 5 ≪ 1 is small enough that U ( | φ | ≤ | φ ⋆ | ) remains approximately quadratic.CC-BY · From the PDF
Image 6
CC-BY · From the PDF
Figure 20 Potential U ( ) Figure 7 . Left: the scalar potential ˆ U ( φ ) , as given in eq. (4.1), for several values of δ ≡ U fv /U 0 , as indicated in the figure. A potential of this kind, exhibiting a de Sitter vacuum that is separated by a finite barrier from the compactification limit, admits hybrid BON-CDL and BON-HM instanton solutions. Right: to illustrate the physical meaning of a , we show ˆ U with fixed δ = 0 . 2 as a function of the proper length of the KK direction, L = 2 πR 5 exp (√ 2 3 φ/M p ) . Larger values of a create a steeper potential near the false vacuum at L = 2 πR 5 , while also flattening U ( L ) at L ≪ πR 5 .
Figure 20 Potential U ( ) Figure 7 . Left: the scalar potential ˆ U ( φ ) , as given in eq. (4.1), for several values of δ ≡ U fv /U 0 , as indicated in the figure. A potential of this kind, exhibiting a de Sitter vacuum that is separated by a finite barrier from the compactification limit, admits hybrid BON-CDL and BON-HM instanton solutions. Right: to illustrate the physical meaning of a , we show ˆ U with fixed δ = 0 . 2 as a function of the proper length of the KK direction, L = 2 πR 5 exp (√ 2 3 φ/M p ) . Larger values of a create a steeper potential near the false vacuum at L = 2 πR 5 , while also flattening U ( L ) at L ≪ πR 5 .CC-BY · From the PDF
Image 8
CC-BY · From the PDF
Figure 14 Parameter space R 3 /R 5 Figure 9 . The trajectories of the BON bounce solutions in the ( η, R 5 ) plane are shown for a = 5 and various 0 < δ < 1 . Each value of δ has a BON-FV branch of solutions, with R 3 ≈ R 5 ( φ 0 ≈ 0 ) in the u 0 ≪ 1 limit where the potential becomes unimportant. The BON-CDL branch of solutions has R 3 < R 5 ( φ 0 ≈ φ cdl ) in the u 0 ≪ 1 limit, and an action ∆ S ≈ S CDL that is large compared to π 2 M 2 p R 2 5 . When u 0 ≳ 1 , the potential U ( φ ) is no longer a small perturbation to the Witten bubble, and we find that the BON-FV and BON-CDL branches merge together, with u 0 for the bounce solution bounded from above by some u max 0 . For u 0 > u max 0 , all solutions to the equations of motion are of the overshoot type. As δ → 0 the CDL action diverges as δ -1 , and the unification of the BON-FV and BON-CDL branches is pushed to ever-larger values of u 0 ≫ 1 .
Figure 14 Parameter space R 3 /R 5 Figure 9 . The trajectories of the BON bounce solutions in the ( η, R 5 ) plane are shown for a = 5 and various 0 < δ < 1 . Each value of δ has a BON-FV branch of solutions, with R 3 ≈ R 5 ( φ 0 ≈ 0 ) in the u 0 ≪ 1 limit where the potential becomes unimportant. The BON-CDL branch of solutions has R 3 < R 5 ( φ 0 ≈ φ cdl ) in the u 0 ≪ 1 limit, and an action ∆ S ≈ S CDL that is large compared to π 2 M 2 p R 2 5 . When u 0 ≳ 1 , the potential U ( φ ) is no longer a small perturbation to the Witten bubble, and we find that the BON-FV and BON-CDL branches merge together, with u 0 for the bounce solution bounded from above by some u max 0 . For u 0 > u max 0 , all solutions to the equations of motion are of the overshoot type. As δ → 0 the CDL action diverges as δ -1 , and the unification of the BON-FV and BON-CDL branches is pushed to ever-larger values of u 0 ≫ 1 .CC-BY · From the PDF
Image 10
CC-BY · From the PDF
Figure 31 ⇢ ( ⇠ ) with inset Left: BON-FV Right: BON-CdL 15 Figure 11 . Profiles for ρ ( ξ ) for U 0 R 2 5 /M 2 p = 0 . 01 on the BON-FV ( left ) and BON-CDL ( right ) branches. For the BON-FV branch the solutions for ρ ( ξ ) are nearly identical to the false vacuum solution ρ fv ( ξ ) for ξ ≳ R 5 . This encompasses the majority of the domain 0 ≤ ξ ≤ ξ max ≈ π Λ , which is why we only show δ = 0 . 001 . . . 0 . 2 . For the BON-CDL solutions, the profiles for ρ ( ξ ) follow the ξ ≫ R 5 linear growth of eq. (2.22) out to ξ ≳ 10 R 5 or larger, with a relatively sharp transition from ρ ′ ≈ 1 to ρ ′ ≈ -1 in the case of small δ . As δ → 1 , the BON-CDL solutions for ρ ( ξ ) more closely match the Hawking-Moss behavior ρ ( ξ ) ≈ ρ HM ( ξ ) for all ξ ≳ R 5 , even though the a = 5 CDL and HM solutions for φ ( ξ ) are distinct.
Figure 31 ⇢ ( ⇠ ) with inset Left: BON-FV Right: BON-CdL 15 Figure 11 . Profiles for ρ ( ξ ) for U 0 R 2 5 /M 2 p = 0 . 01 on the BON-FV ( left ) and BON-CDL ( right ) branches. For the BON-FV branch the solutions for ρ ( ξ ) are nearly identical to the false vacuum solution ρ fv ( ξ ) for ξ ≳ R 5 . This encompasses the majority of the domain 0 ≤ ξ ≤ ξ max ≈ π Λ , which is why we only show δ = 0 . 001 . . . 0 . 2 . For the BON-CDL solutions, the profiles for ρ ( ξ ) follow the ξ ≫ R 5 linear growth of eq. (2.22) out to ξ ≳ 10 R 5 or larger, with a relatively sharp transition from ρ ′ ≈ 1 to ρ ′ ≈ -1 in the case of small δ . As δ → 1 , the BON-CDL solutions for ρ ( ξ ) more closely match the Hawking-Moss behavior ρ ( ξ ) ≈ ρ HM ( ξ ) for all ξ ≳ R 5 , even though the a = 5 CDL and HM solutions for φ ( ξ ) are distinct.CC-BY · From the PDF
Figure 24 Action as function of R 5 Figure 12 . The de Sitter-subtracted Euclidean action ∆ S is shown in units of M 4 p /U 0 as a function of R 5 , for a = 5 and various 0 < δ < 1 . The dashed gray line shows the ∆ S ≈ π 2 M 2 p R 2 5 expectation from the small u 0 ≪ 1 limit of the BON-FV solutions. It tracks the numericallycomputed action closely on this branch for all u 0 ≪ 1 . This branch is always of lowest action and determines the tunneling rate. On the BON-CDL branch the action approaches a constant, the ordinary CDL action ∆ S ≈ S CDL , which is large compared to M 4 p /U 0 for δ ≲ 0 . 5 . For δ ≪ 1 , S CDL ≈ 24 π 2 M 4 p / ( δ · U 0 ) , grows as 1 /δ . At larger values of u 0 , where π 2 M 2 p R 2 5 ∼ ∆ S CDL , the BON-FV and BON-CDL branches of bounce solutions meet. (This method of estimating the value of u 0 = U 0 R 2 5 /M 2 p at which the two branches meet becomes imprecise once u 0 ≳ 1 , where π 2 M 2 p R 5 is no longer a good approximation to the BON-FV action.)
Figure 24 Action as function of R 5 Figure 12 . The de Sitter-subtracted Euclidean action ∆ S is shown in units of M 4 p /U 0 as a function of R 5 , for a = 5 and various 0 < δ < 1 . The dashed gray line shows the ∆ S ≈ π 2 M 2 p R 2 5 expectation from the small u 0 ≪ 1 limit of the BON-FV solutions. It tracks the numericallycomputed action closely on this branch for all u 0 ≪ 1 . This branch is always of lowest action and determines the tunneling rate. On the BON-CDL branch the action approaches a constant, the ordinary CDL action ∆ S ≈ S CDL , which is large compared to M 4 p /U 0 for δ ≲ 0 . 5 . For δ ≪ 1 , S CDL ≈ 24 π 2 M 4 p / ( δ · U 0 ) , grows as 1 /δ . At larger values of u 0 , where π 2 M 2 p R 2 5 ∼ ∆ S CDL , the BON-FV and BON-CDL branches of bounce solutions meet. (This method of estimating the value of u 0 = U 0 R 2 5 /M 2 p at which the two branches meet becomes imprecise once u 0 ≳ 1 , where π 2 M 2 p R 5 is no longer a good approximation to the BON-FV action.)CC-BY · From the PDF
Figure 16 Potential U ( , ⇤ ) Figure 13 . The scalar potential ˆ U λ ( φ ) of eq. (5.4), for several values of λ ≡ Λ CC 5 M 2 p /U 0 .
Figure 16 Potential U ( , ⇤ ) Figure 13 . The scalar potential ˆ U λ ( φ ) of eq. (5.4), for several values of λ ≡ Λ CC 5 M 2 p /U 0 .CC-BY · From the PDF
Image 14
CC-BY · From the PDF
Image 15
CC-BY · From the PDF
Image 16
CC-BY · From the PDF

Verification

Claims the paper makes

The claims and statistics of this paper haven’t been checked yet.

Run the check — free, no account needed. It reads the open-access text and checks the sources it cites.

A few free checks a day · papers already verified open instantly · results are public

Claims other papers make about this one

Each is checked against this paper’s own text: does it say what the citing paper says it does?

Self-check

Percentages, sums and reported differences re-computed from the paper’s own numbers.

The self-check needs the paper’s full text.

Citations

Cites

Show all 9 references

Research works printed but not linked: 47

  1. Supernova Cosmology Project collaboration, Measurements of Ω and Λ from 42 high redshift supernovae, Astrophys. J. 517 (1999) 565 [astro-ph/9812133] [INSPIRE]. · arXiv
  2. SDSS collaboration, Baryon acoustic oscillations in the Sloan Digital Sky Survey data release 7 galaxy sample, Mon. Not. Roy. Astron. Soc. 401 (2010) 2148 [arXiv:0907.1660] [INSPIRE]. · arXiv
  3. Planck collaboration, Planck 2018 results. VI. Cosmological parameters, Astron. Astrophys. 641 (2020) A6 [Erratum ibid. 652 (2021) C4] [arXiv:1807.06209] [INSPIRE]. · arXiv
  4. S. Kachru, R. Kallosh, A. D. Linde and S. P. Trivedi, De Sitter vacua in string theory, Phys. Rev. D 68 (2003) 046005 [hep-th/0301240] [INSPIRE]. · DOI
  5. V. Balasubramanian, P. Berglund, J. P. Conlon and F. Quevedo, Systematics of moduli stabilisation in Calabi-Yau flux compactifications, JHEP 03 (2005) 007 [hep-th/0502058] [INSPIRE]. · DOI · Paper page
  6. J. M. Maldacena and C. Núñez, Supergravity description of field theories on curved manifolds and a no go theorem, Int. J. Mod. Phys. A 16 (2001) 822 [hep-th/0007018] [INSPIRE]. · DOI · Paper page
  7. P. K. Townsend, Cosmic acceleration and M-theory, in 14th International congress on mathematical physics, (2003), pg. 655 [hep-th/0308149] [INSPIRE]. · arXiv
  8. M. P. Hertzberg, S. Kachru, W. Taylor and M. Tegmark, Inflationary constraints on type IIA string theory, JHEP 12 (2007) 095 [arXiv:0711.2512] [INSPIRE]. · DOI · Paper page
  9. T. Wrase and M. Zagermann, On classical de Sitter vacua in string theory, Fortsch. Phys. 58 (2010) 906 [arXiv:1003.0029] [INSPIRE]. · DOI
  10. G. Shiu and Y. Sumitomo, Stability constraints on classical de Sitter vacua, JHEP 09 (2011) 052 [arXiv:1107.2925] [INSPIRE]. · DOI
  11. I. Bena, M. Graña, S. Kuperstein and S. Massai, Giant tachyons in the landscape, JHEP 02 (2015) 146 [arXiv:1410.7776] [INSPIRE]. · DOI
  12. D. Kutasov, T. Maxfield, I. Melnikov and S. Sethi, Constraining de Sitter space in string theory, Phys. Rev. Lett. 115 (2015) 071305 [arXiv:1504.00056] [INSPIRE]. · DOI
  13. D. Andriot and J. Blåbäck, Refining the boundaries of the classical de Sitter landscape, JHEP 03 (2017) 102 [Erratum ibid. 03 (2018) 083] [arXiv:1609.00385] [INSPIRE]. · DOI
  14. J. Moritz, A. Retolaza and A. Westphal, Toward de Sitter space from ten dimensions, Phys. Rev. D 97 (2018) 046010 [arXiv:1707.08678] [INSPIRE]. · DOI
  15. S. Sethi, Supersymmetry breaking by fluxes, JHEP 10 (2018) 022 [arXiv:1709.03554] [INSPIRE]. · DOI
  16. U. H. Danielsson and T. Van Riet, What if string theory has no de Sitter vacua?, Int. J. Mod. Phys. D 27 (2018) 1830007 [arXiv:1804.01120] [INSPIRE]. · DOI
  17. Y. Hamada, A. Hebecker, G. Shiu and P. Soler, On brane gaugino condensates in 10d, JHEP 04 (2019) 008 [arXiv:1812.06097] [INSPIRE]. · DOI
  18. Y. Hamada, A. Hebecker, G. Shiu and P. Soler, Understanding KKLT from a 10d perspective, JHEP 06 (2019) 019 [arXiv:1902.01410] [INSPIRE]. · DOI
  19. F. Carta, J. Moritz and A. Westphal, Gaugino condensation and small uplifts in KKLT, JHEP 08 (2019) 141 [arXiv:1902.01412] [INSPIRE]. · DOI
  20. X. Gao, A. Hebecker and D. Junghans, Control issues of KKLT, Fortsch. Phys. 68 (2020) 2000089 [arXiv:2009.03914] [INSPIRE]. · DOI
  21. I. Basile and S. Lanza, De Sitter in non-supersymmetric string theories: no-go theorems and brane-worlds, JHEP 10 (2020) 108 [arXiv:2007.13757] [INSPIRE]. · DOI
  22. G. Obied, H. Ooguri, L. Spodyneiko and C. Vafa, De Sitter space and the swampland, arXiv:1806.08362 [INSPIRE]. · arXiv
  23. S. K. Garg and C. Krishnan, Bounds on slow roll and the de Sitter swampland, JHEP 11 (2019) 075 [arXiv:1807.05193] [INSPIRE]. · DOI
  24. H. Ooguri, E. Palti, G. Shiu and C. Vafa, Distance and de Sitter conjectures on the swampland, Phys. Lett. B 788 (2019) 180 [arXiv:1810.05506] [INSPIRE]. · DOI
  25. A. Bedroya and C. Vafa, Trans-Planckian censorship and the swampland, JHEP 09 (2020) 123 [arXiv:1909.11063] [INSPIRE]. · DOI
  26. S. B. Giddings, The fate of four-dimensions, Phys. Rev. D 68 (2003) 026006 [hep-th/0303031] [INSPIRE]. · DOI · Paper page
  27. M. Dine, P. J. Fox and E. Gorbatov, Catastrophic decays of compactified space-times, JHEP 09 (2004) 037 [hep-th/0405190] [INSPIRE]. · DOI
  28. M. Fabinger and P. Hořava, Casimir effect between world branes in heterotic M-theory, Nucl. Phys. B 580 (2000) 243 [hep-th/0002073] [INSPIRE]. · DOI · Paper page
  29. D. Brill and G. T. Horowitz, Negative energy in string theory, Phys. Lett. B 262 (1991) 437 [INSPIRE]. · DOI · Paper page
  30. S. P. De Alwis and A. T. Flournoy, Closed string tachyons and semiclassical instabilities, Phys. Rev. D 66 (2002) 026005 [hep-th/0201185] [INSPIRE]. · DOI · Paper page
  31. B. S. Acharya, Supersymmetry, Ricci flat manifolds and the string landscape, JHEP 08 (2020) 128 [arXiv:1906.06886] [INSPIRE]. · DOI · Paper page
  32. G. T. Horowitz, J. Orgera and J. Polchinski, Nonperturbative instability of AdS5 × S5/Zk, Phys. Rev. D 77 (2008) 024004 [arXiv:0709.4262] [INSPIRE]. · DOI
  33. J. J. Blanco-Pillado and B. Shlaer, Bubbles of nothing in flux compactifications, Phys. Rev. D 82 (2010) 086015 [arXiv:1002.4408] [INSPIRE]. · DOI
  34. A. R. Brown and A. Dahlen, Bubbles of nothing and the fastest decay in the landscape, Phys. Rev. D 84 (2011) 043518 [arXiv:1010.5240] [INSPIRE]. · DOI · Paper page
  35. J. J. Blanco-Pillado, H. S. Ramadhan and B. Shlaer, Decay of flux vacua to nothing, JCAP 10 (2010) 029 [arXiv:1009.0753] [INSPIRE]. · DOI
  36. H. Ooguri and L. Spodyneiko, New Kaluza-Klein instantons and the decay of AdS vacua, Phys. Rev. D 96 (2017) 026016 [arXiv:1703.03105] [INSPIRE]. · DOI · Paper page
  37. P. Draper, I. G. Garcia and B. Lillard, Bubble of nothing decays of unstable theories, Phys. Rev. D 104 (2021) L121701 [arXiv:2105.08068] [INSPIRE]. · DOI · Paper page
  38. S. R. Coleman, The fate of the false vacuum. 1. Semiclassical theory, Phys. Rev. D 15 (1977) 2929 [Erratum ibid. 16 (1977) 1248] [INSPIRE]. · DOI · Paper page
  39. C. G. Callan, Jr. and S. R. Coleman, The fate of the false vacuum. 2. First quantum corrections, Phys. Rev. D 16 (1977) 1762 [INSPIRE]. · DOI · Paper page
  40. L. G. Jensen and P. J. Steinhardt, Bubble nucleation and the Coleman-Weinberg model, Nucl. Phys. B 237 (1984) 176 [INSPIRE]. · DOI
  41. L. G. Jensen and P. J. Steinhardt, Bubble nucleation for flat potential barriers, Nucl. Phys. B 317 (1989) 693 [INSPIRE]. · DOI
  42. J. C. Hackworth and E. J. Weinberg, Oscillating bounce solutions and vacuum tunneling in de Sitter spacetime, Phys. Rev. D 71 (2005) 044014 [hep-th/0410142] [INSPIRE]. · DOI
  43. P. Batra and M. Kleban, Transitions between de Sitter minima, Phys. Rev. D 76 (2007) 103510 [hep-th/0612083] [INSPIRE]. · DOI
  44. P. Draper and S. Farkas, Transplanckian censorship and the local swampland distance conjecture, JHEP 01 (2020) 133 [arXiv:1910.04804] [INSPIRE]. · DOI
  45. A. R. Brown and A. Dahlen, On ‘nothing’ as an infinitely negatively curved spacetime, Phys. Rev. D 85 (2012) 104026 [arXiv:1111.0301] [INSPIRE]. · DOI
  46. C. Angelantonj, M. Cardella and N. Irges, An alternative for moduli stabilisation, Phys. Lett. B 641 (2006) 474 [hep-th/0608022] [INSPIRE]. · DOI
  47. A. Rajantie and S. Stopyra, Standard Model vacuum decay in a de Sitter background, Phys. Rev. D 97 (2018) 025012 [arXiv:1707.09175] [INSPIRE]. · DOI

Cited by

Metadata

Authors
Draper, P., Garcia, I. G., & Lillard, B.
Venue
Journal of High Energy Physics
Publisher
Springer Science and Business Media LLC
Published
2021-12-21
Volume
2021
Issue
12
ISSN
1029-8479
DOI
10.1007/jhep12(2021)154
Cited by
14
References
9
Language
en
Licence

About these checks

Registry, retraction, Cites and statistics results are computed, not judged, with one exception: a printed reference that no index lists is read once by a model before it counts as a citation error. Claims are extracted by a model and kept only when their quote appears verbatim in the text; each cited source is then checked, with a model’s help, for whether it says what the claim relies on. Those verdicts can be wrong — read the claim’s quote and the cited source before relying on one.

Statistics and arithmetic are recomputed, not judged.

Confidence bands are shown only for fields calibrated on our annotated test set. None is calibrated yet, so no band is shown.

What counts as a claim ›How we measure confidence ›How we check this ›

Are you an author, or do you see a problem with this page? Request a review

Data sources

Bibliographic data: Semantic Scholar, OpenAlex, Crossref.

Contains information from the Semantic Scholar Academic Graph Datasets, made available under the ODC Attribution License (ODC-BY 1.0).

Semantic Scholar’s data is described in: Kinney, R., et al. (2023). The Semantic Scholar Open Data Platform. arXiv:2301.10140.