Export citation

Export citation

Choose format for download:

Download Citation
  • Access by Xinjiang University

Heavy quark production in the Aivazis-Collins-Olness-Tung scheme at next-to-next-to-leading and next-to-next-to-next-to-leading order

T. Stavreva1,*, F. I. Olness2,†, I. Schienbein1,‡, T. Ježo1,§, A. Kusina2,∥, K. Kovařík3,¶, and J. Y. Yu2,1,**

  • 1Laboratoire de Physique Subatomique et de Cosmologie, Université Joseph Fourier/CNRS-IN2P3/INPG, 53 Avenue des Martyrs, 38026 Grenoble, France
  • 2Southern Methodist University, Dallas, Texas 75275, USA
  • 3Institute for Theoretical Physics, Karlsruhe Institute of Technology, Karlsruhe, D-76128, Germany

  • *stavreva@lpsc.in2p3.fr
  • olness@smu.edu
  • schien@lpsc.in2p3.fr
  • §jezo@lpsc.in2p3.fr
  • akusina@smu.edu
  • kovarik@particle.uni-karlsruhe.de
  • **yu@physics.smu.edu

Phys. Rev. D 85, 114014 – Published 7 June, 2012

DOI: https://doi.org/10.1103/PhysRevD.85.114014

Abstract

We analyze the properties of the Aivazis-Collins-Olness-Tung (ACOT) scheme for heavy quark production and make use of the MS¯ massless results at next-to-next-to-leading order and N3LO for the structure functions F2 and FL in neutral current deep-inelastic scattering to estimate the higher order corrections. For this purpose we decouple the heavy quark mass entering the phase space from the one entering the dynamics of the short distance cross section. We show numerically that the phase space mass is generally more important. Therefore, the dominant heavy quark mass effects at higher orders can be taken into account using the massless Wilson coefficients together with an appropriate slow-rescaling prescription implementing the phase space constraints. Combining the exact ACOT scheme at next-to-leading order with these expressions should provide a good approximation to the missing full calculation in the ACOT scheme at next-to-next-to-leading order and N3LO.

Article Text

References (42)

  1. I. Schienbein et al., J. Phys. G 35, 053101 (2008).
  2. H1 and ZEUS Collaborations, Report Nos. H1prelim-10-044 and ZEUS-prel-10-008, 2010 (unpublished), http://www-h1.desy.de/psfiles/confpap/DIS2010/H1prelim-10-044.pdf.
  3. F. D. Aaron et al., Eur. Phys. J. C 71, 1579 (2011).
  4. M. A. G. Aivazis, J. C. Collins, F. I. Olness, and W. K. Tung, Phys. Rev. D 50, 3102 (1994).
  5. J. C. Collins, Phys. Rev. D 58, 094002 (1998).
  6. S. Kretzer and I. Schienbein, Phys. Rev. D 58, 094035 (1998).
  7. R. Thorne and R. Roberts, Phys. Lett. B 421, 303 (1998).
  8. M. Krämer, F. I. Olness, and D. E. Soper, Phys. Rev. D 62, 096007 (2000).
  9. R. M. Barnett, Phys. Rev. Lett. 36, 1163 (1976).
  10. W. K. Tung, S. Kretzer, and C. Schmidt, J. Phys. G 28, 983 (2002).
  11. S. Kretzer, H. Lai, F. Olness, and W. Tung, Phys. Rev. D 69, 114005 (2004).
  12. M. Guzzi, P. M. Nadolsky, H.-L. Lai, and C.-P. Yuan, arXiv:1108.5112.
  13. E. Laenen, S. Riemersma, J. Smith, and W. L. van Neerven, Nucl. Phys. B392, 162 (1993).
  14. M. Guzzi, P. M. Nadolsky, H.-L. Lai, and C. P. Yuan, arXiv:1108.4008.
  15. R. Thorne and R. Roberts, Phys. Rev. D 57, 6871 (1998).
  16. R. Thorne, Phys. Rev. D 73, 054019 (2006).
  17. M. Cacciari, M. Greco, and P. Nason, J. High Energy Phys. 05 (1998) 007.
  18. S. Forte, E. Laenen, P. Nason, and J. Rojo, Nucl. Phys. B834, 116 (2010).
  19. R. D. Ball et al. (NNPDF Collaboration), Nucl. Phys. B849, 296 (2011).
  20. J. Andersen et al. (SM and NLO Multileg Working Group), arXiv:1003.1241.
  21. T. Gottschalk, Phys. Rev. D 23, 56 (1981).
  22. M. Gluck, S. Kretzer, and E. Reya, Phys. Lett. B 380, 171 (1996).
  23. J. Blumlein, A. Hasselhuhn, P. Kovacikova, and S. Moch, Phys. Lett. B 700, 294 (2011).
  24. M. Buza and W. van Neerven, Nucl. Phys. B500, 301 (1997).
  25. W. Furmanski and R. Petronzio, Z. Phys. C 11, 293 (1982).
  26. W. A. Bardeen, A. J. Buras, D. W. Duke, and T. Muta, Phys. Rev. D 18, 3998 (1978).
  27. G. Altarelli, R. K. Ellis, and G. Martinelli, Nucl. Phys. B143, 521 (1978).
  28. W. L. van Neerven and E. B. Zijlstra, Phys. Lett. B 272, 127 (1991).
  29. E. B. Zijlstra and W. L. van Neerven, Phys. Lett. B 273, 476 (1991).
  30. E. B. Zijlstra and W. L. van Neerven, Nucl. Phys. B383, 525 (1992).
  31. J. A. M. Vermaseren, A. Vogt, and S. Moch, Nucl. Phys. B724, 3 (2005).
  32. W. L. van Neerven and A. Vogt, Nucl. Phys. B568, 263 (2000).
  33. W. L. van Neerven and A. Vogt, Nucl. Phys. B588, 345 (2000).
  34. S. Moch, J. A. M. Vermaseren, and A. Vogt, Nucl. Phys. B646, 181 (2002).
  35. J. Sanchez Guillen, J. Miramontes, M. Miramontes, G. Parente, and O. A. Sampayo, Nucl. Phys. B353, 337 (1991).
  36. S. Moch, J. A. M. Vermaseren, and A. Vogt, Phys. Lett. B 606, 123 (2005).
  37. M. A. G. Aivazis, F. I. Olness, and W. K. Tung, Phys. Rev. D 50, 3085 (1994).
  38. M. Botje, Comput. Phys. Commun. 182, 490 (2011).
  39. W. Giele et al., hep-ph/0204316.
  40. A. Chuvakin, J. Smith, and W. L. van Neerven, Phys. Rev. D 61, 096004 (2000).
  41. M. Buza, Y. Matiounine, J. Smith, R. Migneron, and W. van Neerven, Nucl. Phys. B472, 611 (1996).
  42. F. I. Olness and R. J. Scalise, Phys. Rev. D 57, 241 (1998).

Outline

Information

Sign In to Your Journals Account

Filter

Filter

Article Lookup

Enter a citation