CoChat
Sign Up
Cited by 62Stellar, planetary, and galactic studiesGalaxies: Formation, Evolution, PhenomenaAstronomy and Astrophysical Research

THE ROLE OF THERMOHALINE MIXING IN INTERMEDIATE- AND LOW-METALLICITY GLOBULAR CLUSTERS

Open access
Angelou, George C., Stancliffe, Richard J., Church, Ross P., Lattanzio, John C., Smith, Graeme H.·2012·The Astrophysical Journal
DOI 10.1088/0004-637x/749/2/128
Open this paper in CoChat — free accountOpen PDF

Abstract

It is now widely accepted that globular cluster red giant branch (RGB) stars owe their strange abundance patterns to a combination of pollution from progenitor stars and in situ extra mixing. In this hybrid theory a first generation of stars imprints abundance patterns into the gas from which a second generation forms. The hybrid theory suggests that extra mixing is operating in both populations and we use the variation of [C/Fe] with luminosity to examine how efficient this mixing is. We investigate the observed RGBs of M3, M13, M92, M15, and NGC 5466 as a means to test a theory of thermohaline mixing. The second parameter pair M3 and M13 are of intermediate metallicity and our models are able to account for the evolution of carbon along the RGB in both clusters, although in order to fit the most carbon-depleted main-sequence stars in M13 we require a model whose initial [C/Fe] abundance leads to a carbon abundance lower than is observed. Furthermore, our results suggest that stars in M13 formed with some primary nitrogen (higher C+N+O than stars in M3). In the metal-poor regime only NGC 5466 can be tentatively explained by thermohaline mixing operating in multiple populations. We find thermohaline mixing unable to model the depletion of [C/Fe] with magnitude in M92 and M15. It appears as if extra mixing is occurring before the luminosity function bump in these clusters. To reconcile the data with the models would require first dredge-up to be deeper than found in extant models.

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 · 10.1088/0004-637x/749/2/128

Cites

1 of 1 references verified0 citation errors · 0 not checkable

Statistics

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?

  • In the metal-poor globular cluster M92, the data show a clear decrease in [C/Fe] with increasing luminosity on the RGB starting at MV≈12, well before the bump at MV≈-0.5, a substantial disagreement.

    “Here the data show a clear decrease in [ C/Fe ] with increasing luminosity on the RGB (Bellman et al. 2001; Smith & Martell 2003), starting at MV ≈ 12. The problem is that the decrease begins well before the bump in the LF, which Martell, Smith, & Briley (2008) place at MV ≈ -0 . 5. This is a substantial disagreement.”

    From The Dawes Review 2: Nucleosynthesis and Stellar Yields of Low- and Intermediate-Mass Single Stars (2014) · cites this paper as Angelou et al. 2012

    Section 2.2.2 (M92; page unavailable) says carbon abundances turn down before the luminosity-function bump, although it describes the depletion as apparent and notes a large spread in [C/Fe]. Section 3.1 (page unavailable) reports Martell et al.’s bump estimate as M_V ≈ −0.55, consistent with ≈ −0.5. The cited paper does not establish the claimed onset at M_V ≈ 12. (LLM, conf=0.86)

    Experimental — accuracy not yet measured

Self-check

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

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

Cites

Flagged first, then by citations

Research works printed but not linked: 129

  1. Anderson, J., Piotto, G., King, I. R., Bedin, L. R., & Guhathakurta, P. 2009, ApJ, 697, L58 · DOI
  2. Angelou, G. C., Church, R. P., Stancliffe, R. J., Lattanzio, J. C., & Smith, G. H. 2011, ApJ, 728, 79 · DOI
  3. Arp, H. C. 1955, AJ, 60, 317 · DOI
  4. Arp, H. C., Baum, W. A., & Sandage, A. R. 1952, AJ, 57, 4 · DOI
  5. Bazán, G., Dearborn, D. S. P., Dossa, D. D., et al. 2003, in ASP Conf. Ser. 293, 3D Stellar Evolution, ed. S. Turcotte, S. C. Keller, & R. M. Cavallo (San Francisco, CA: ASP), 1
  6. Bellman, S., Briley, M. M., Smith, G. H., & Claver, C. F. 2001, PASP, 113, 326 · DOI · Paper page
  7. Briley, M. M., & Cohen, J. G. 2001, AJ, 122, 242 · DOI
  8. Briley, M. M., Cohen, J. G., & Stetson, P. B. 2002, ApJ, 579, L17 · DOI
  9. Briley, M. M., Cohen, J. G., & Stetson, P. B. 2004, AJ, 127, 1579 · DOI
  10. Briley, M. M., Hesser, J. E., & Bell, R. A. 1991, ApJ, 373, 482 · DOI
  11. Brown, J. A., & Wallerstein, G. 1993, AJ, 106, 133 · DOI
  12. Busso, M., Wasserburg, G. J., Nollett, K. M., & Calandra, A. 2007, ApJ, 671, 802 · DOI · Paper page
  13. Campbell, S. W., & Lattanzio, J. C. 2008, A&A, 490, 769 · DOI
  14. Cannon, R. D., Croke, B. F. W., Bell, R. A., Hesser, J. E., & Stathakis, R. A. 1998, MNRAS, 298, 601 · DOI
  15. Cantiello, M., & Langer, N. 2010, A&A, 521, A9 · DOI
  16. Carbon, D. F., Romanishin, W., Langer, G. E., et al. 1982, ApJS, 49, 207 · DOI
  17. Catelan, M., Borissova, J., Ferraro, F. R., et al. 2002, AJ, 124, 364 · DOI
  18. Chaboyer, B., Sarajedini, A., & Demarque, P. 1992, ApJ, 394, 515 · DOI
  19. Chanamé, J., Pinsonneault, M., & Terndrup, D. M. 2005, ApJ, 631, 540 · DOI · Paper page
  20. Charbonnel, C. 1995, ApJ, 453, L41 · DOI · Paper page
  21. Charbonnel, C. 2010, IAUS, 266, 131 · DOI
  22. Charbonnel, C., & Lagarde, N. 2010, A&A, 522, A10 · DOI
  23. Charbonnel, C., & Zahn, J. 2007a, A&A, 467, L15 · DOI
  24. Charbonnel, C., & Zahn, J. 2007b, A&A, 476, L29 · DOI
  25. Cohen, J. G. 1978, ApJ, 223, 487 · DOI
  26. Cohen, J. G. 1999, AJ, 117, 2428 · DOI
  27. Cohen, J. G. 2011, ApJ, 740, L38 · DOI
  28. Cohen, J. G., & Meléndez, J. 2005, AJ, 129, 303 · DOI
  29. D'Antona, F., Bellazzini, M., Caloi, V., et al. 2005, ApJ, 631, 868 · DOI
  30. D'Antona, F., & Caloi, V. 2008, MNRAS, 390, 693 · DOI
  31. Decressin, T., Meynet, G., Charbonnel, C., Prantzos, N., & Ekström, S. 2007, A&A, 464, 1029 · DOI
  32. de Mink, S. E., Pols, O. R., Langer, N., & Izzard, R. G. 2009, A&A, 507, L1 · DOI
  33. Denissenkov, P. A. 2010, ApJ, 723, 563 · DOI
  34. Denissenkov, P. A., Chaboyer, B., & Li, K. 2006, ApJ, 641, 1087 · DOI
  35. Denissenkov, P. A., & Merryfield, W. J. 2011, ApJ, 727, L8 · DOI
  36. Denissenkov, P. A., & Pinsonneault, M. 2008a, ApJ, 679, 1541 · DOI
  37. Denissenkov, P. A., & Pinsonneault, M. 2008b, ApJ, 684, 626 · DOI
  38. Denissenkov, P. A., Pinsonneault, M., & MacGregor, K. B. 2009, ApJ, 696, 1823 · DOI · Paper page
  39. Denissenkov, P. A., & Tout, C. A. 2000, MNRAS, 316, 395 · DOI
  40. Denissenkov, P. A., & VandenBerg, D. A. 2003, ApJ, 593, 509 · DOI
  41. di Cecco, A., Becucci, R., Bono, G., et al. 2010, PASP, 122, 991 · DOI
  42. Eggleton, P. P., Dearborn, D. S. P., & Lattanzio, J. C. 2006, Science, 314, 1580 · DOI · Paper page
  43. Eggleton, P. P., Dearborn, D. S. P., & Lattanzio, J. C. 2008, ApJ, 677, 581 · DOI
  44. Fekadu, N., Sandquist, E. L., & Bolte, M. 2007, ApJ, 663, 277 · DOI
  45. Fenner, Y., Campbell, S., Karakas, A. I., Lattanzio, J. C., & Gibson, B. K. 2004, MNRAS, 353, 789 · DOI · Paper page
  46. Gnedin, O. Y., & Ostriker, J. P. 1997, ApJ, 474, 223 · DOI
  47. Gratton, R., Sneden, C., & Carretta, E. 2004, ARA&A, 42, 385 · DOI · Paper page
  48. Gratton, R. G., Fusi Pecci, F., Carretta, E., et al. 1997, ApJ, 491, 749 · DOI
  49. Grundahl, F., VandenBerg, D. A., Bell, R. A., Andersen, M. I., & Stetson, P. B. 2000, AJ, 120, 1884 · DOI
  50. Harris, W. E. 1996, AJ, 112, 1487 · DOI · Paper page
  51. Hata, N., Scherrer, R. J., Steigman, G., et al. 1995, Phys. Rev. Lett., 75, 3977 · DOI
  52. Herwig, F. 2005, ARA&A, 43, 435 · DOI
  53. Hesser, J. E., & Bell, R. A. 1980, ApJ, 238, L149 · DOI
  54. Hogan, C. J. 1995, ApJ, 441, L17 · DOI
  55. Hubbard, E. N., & Dearborn, D. S. P. 1980, ApJ, 239, 248 · DOI
  56. Iben, I., Jr. 1967, ApJ, 147, 624 · DOI
  57. Iben, I., Jr., & Ehrman, J. R. 1962, ApJ, 135, 770 · DOI
  58. Iben, I., Jr., & Faulkner, J. 1968, ApJ, 153, 101 · DOI
  59. Johnson, H. L., & Sandage, A. R. 1955, ApJ, 121, 616 · DOI
  60. Kraft, R. P. 1994, PASP, 106, 553 · DOI
  61. Kraft, R. P., Sneden, C., Langer, G. E., & Prosser, C. F. 1992, AJ, 104, 645 · DOI
  62. Lagarde, N., Charbonnel, C., Decressin, T., & Hagelberg, J. 2011, A&A, 536, A28 · DOI
  63. Langer, G. E., Kraft, R. P., Carbon, D. F., Friel, E., & Oke, J. B. 1986, PASP, 98, 473 · DOI
  64. Lee, S. 1999, AJ, 118, 920 · DOI
  65. Lee, Y., Joo, S.-J., Han, S.-I., et al. 2005, ApJ, 621, L57 · DOI
  66. Lind, K., Primas, F., Charbonnel, C., Grundahl, F., & Asplund, M. 2009, A&A, 503, 545 · DOI
  67. Martell, S. L., Smith, G. H., & Briley, M. M. 2008a, PASP, 120, 7 · DOI
  68. Martell, S. L., Smith, G. H., & Briley, M. M. 2008b, AJ, 136, 2522 · DOI
  69. Mucciarelli, A., Salaris, M., Lovisi, L., et al. 2011, MNRAS, 412, 81 · DOI
  70. Nataf, D. M., Gould, A. P., Pinsonneault, M. H., & Udalski, A. 2011, arXiv:1109.2118 · arXiv
  71. Nordhaus, J., Busso, M., Wasserburg, G. J., Blackman, E. G., & Palmerini, S. 2008, ApJ, 684, L29 · DOI · Paper page
  72. Norris, J., Cottrell, P. L., Freeman, K. C., & Da Costa, G. S. 1981, ApJ, 244, 205 · DOI
  73. Norris, J., & Pilachowski, C. A. 1985, ApJ, 299, 295 · DOI
  74. Norris, J., & Smith, G. H. 1984, ApJ, 287, 255 · DOI
  75. Oke, J. B., & Schwarzschild, M. 1952, ApJ, 116, 317 · DOI
  76. Palacios, A., Charbonnel, C., Talon, S., & Siess, L. 2006, A&A, 453, 261 · DOI
  77. Palmerini, S., Busso, M., Maiorca, E., & Guandalini, R. 2009, PASA, 26, 161 · DOI · Paper page
  78. Palmerini, S., Cristallo, S., Busso, M., et al. 2011a, ApJ, 741, 26 · DOI
  79. Palmerini, S., La Cognata, M., Cristallo, S., & Busso, M. 2011b, ApJ, 729, 3 · DOI · Paper page
  80. Pancino, E., Rejkuba, M., Zoccali, M., & Carrera, R. 2010, A&A, 524, A44 · DOI
  81. Paust, N. E. Q., Chaboyer, B., & Sarajedini, A. 2007, AJ, 133, 2787 · DOI
  82. Pavlenko, Y. V., Jones, H. R. A., & Longmore, A. J. 2003, MNRAS, 345, 311 · DOI
  83. Peterson, R. C. 1980, ApJ, 237, L87 · DOI
  84. Peterson, R. C. 1983, ApJ, 275, 737 · DOI
  85. Pilachowski, C., Sneden, C., Freeland, E., & Casperson, J. 2003, AJ, 125, 794 · DOI
  86. Piotto, G. 2009, IAUS, 258, 233 · DOI
  87. Piotto, G., Bedin, L. R., Anderson, J., et al. 2007, ApJ, 661, L53 · DOI
  88. Piotto, G., Villanova, S., Bedin, L. R., et al. 2005, ApJ, 621, 777 · DOI · Paper page
  89. Popper, D. M. 1947, ApJ, 105, 204 · DOI
  90. Recio-Blanco, A., & de Laverny, P. 2007, A&A, 461, L13 · DOI
  91. Reid, I. N. 1997, AJ, 114, 161 · DOI
  92. Roederer, I. U. 2011, ApJ, 732, L17 · DOI
  93. Roederer, I. U., & Sneden, C. 2011, AJ, 142, 22 · DOI
  94. Romano, D., Tosi, M., Matteucci, F., & Chiappini, C. 2003, MNRAS, 346, 295 · DOI
  95. Rood, R. T., Bania, T. M., & Wilson, T. L. 1984, ApJ, 280, 629 · DOI
  96. Salaris, M., & Weiss, A. 2002, A&A, 388, 492 · DOI
  97. Sandage, A. R. 1953, AJ, 58, 61 · DOI
  98. Shetrone, M., Martell, S. L., Wilkerson, R., et al. 2010, AJ, 140, 1119 · DOI
  99. Shetrone, M. D. 2003, ApJ, 585, L45 · DOI
  100. Smith, G. H. 2002, PASP, 114, 1097 · DOI
  101. Smith, G. H. 2006, PASP, 118, 1225 · DOI
  102. Smith, G. H., Briley, M. M., & Harbeck, D. 2005, AJ, 129, 1589 · DOI
  103. Smith, G. H., & Martell, S. L. 2003, PASP, 115, 1211 · DOI
  104. Smith, G. H., Shetrone, M. D., Bell, R. A., Churchill, C. W., & Briley, M. M. 1996, AJ, 112, 1511 · DOI
  105. Smolinski, J. P., Martell, S. L., Beers, T. C., & Lee, Y. S. 2011, AJ, 142, 1268 · DOI
  106. Sneden, C., Kraft, R. P., Guhathakurta, P., Peterson, R. C., & Fulbright, J. P. 2004, AJ, 127, 2162 · DOI
  107. Sneden, C., Kraft, R. P., Prosser, C. F., & Langer, G. E. 1992, AJ, 104, 2121 · DOI
  108. Sneden, C., Kraft, R. P., Shetrone, M. D., et al. 1997, AJ, 114, 1964 · DOI
  109. Sneden, C., Pilachowski, C. A., & Kraft, R. P. 2000, AJ, 120, 1351 · DOI
  110. Sneden, C., Pilachowski, C. A., & Vandenberg, D. A. 1986, ApJ, 311, 826 · DOI
  111. Sollima, A., Ferraro, F. R., Bellazzini, M., et al. 2007, ApJ, 654, 915 · DOI
  112. Spite, M., Cayrel, R., Plez, B., et al. 2005, A&A, 430, 655 · DOI
  113. Spite, M., Cayrel, R., Hill, V., et al. 2006, A&A, 455, 291 · DOI
  114. Stancliffe, R. J. 2010, MNRAS, 403, 505 · DOI · Paper page
  115. Stancliffe, R. J., Church, R. P., Angelou, G. C., & Lattanzio, J. C. 2009, MNRAS, 396, 2313 · DOI · Paper page
  116. Stern, M. 1960, Tellus, 12, 172 · DOI
  117. Suntzeff, N. B. 1981, ApJS, 47, 1 · DOI
  118. Suntzeff, N. B., & Smith, V. V. 1991, ApJ, 381, 160 · DOI
  119. Sweigart, A. V., & Mengel, J. G. 1979, ApJ, 229, 624 · DOI · Paper page
  120. Tosi, M. 1998, Space Sci. Rev., 84, 207 · DOI
  121. Traxler, A., Garaud, P., & Stellmach, S. 2011, ApJ, 728, L29 · DOI
  122. Trefzger, D. V., Langer, G. E., Carbon, D. F., Suntzeff, N. B., & Kraft, R. P. 1983, ApJ, 266, 144 · DOI
  123. Turcotte, S., Bazan, G., Castor, J., et al. 2002, in ASP Conf. Ser. 259, IAU Colloq. 185: Radial and Nonradial Pulsations as Probes of Stellar Physics, ed. C. Aerts, T. R. Bedding, & J. Christensen-Dalsgaard (San Francisco, CA: ASP), 72
  124. Ulrich, R. K. 1972, ApJ, 172, 165 · DOI · Paper page
  125. VandenBerg, D. A. 2000, ApJS, 129, 315 · DOI
  126. Ventura, P., & D'Antona, F. 2011, MNRAS, 410, 2760 · DOI
  127. Wachlin, F. C., Miller Bertolami, M. M., & Althaus, L. G. 2011, A&A, 533, A139 · DOI
  128. Wasserburg, G. J., Boothroyd, A. I., & Sackmann, I. 1995, ApJ, 447, L37 · DOI · Paper page
  129. Zoccali, M., Cassisi, S., Piotto, G., Bono, G., & Salaris, M. 1999, ApJ, 518, L49 · DOI

Cited by

Sorted by citations

Authors
Angelou, G. C., Stancliffe, R. J., Church, R. P., Lattanzio, J. C., & Smith, G. H.
Affiliations
  • Monash University (AU)
  • Mount Stromlo Observatory (AU)
  • Lund University (SE)
  • University of California, Santa Cruz (US)
Corresponding author
Angelou, George C.
ORCID
Venue
The Astrophysical Journal
Publisher
American Astronomical Society
Published
2012-03-30
Volume
749
Issue
2
Pages
128
ISSN
  • 0004-637X (ISSN-L)
  • 1538-4357
DOI
10.1088/0004-637x/749/2/128
OpenAlex
W2090921405
Cited by
62
References
1
Citations by year
2026: 1 · 2025: 1 · 2022: 3 · 2021: 2 · 2020: 4 · 2019: 2 · 2018: 3 · 2017: 8 · 2016: 14 · 2015: 5 · 2014: 8 · 2013: 8 · 2012: 3
FWCI
4.20
Type
journal article
Language
en
Open access
Locations
  • The Astrophysical Journal (publishedVersion)
  • arXiv (Cornell University) (submittedVersion)
  • Lund University Publications (Lund University) (submittedVersion, other-oa)
  • ANU Open Research (Australian National University) (submittedVersion)
  • arXiv (Cornell University)
Funders
  • European Commission (252431)
  • Australian Research Council (DP0879472)
  • National Cancer Institute
Topics
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
  • Physical Sciences › Physics and Astronomy › Instrumentation › Astronomy and Astrophysical Research
Keywords
thermohaline mixing, globular clusters, multiple stellar populations, red giant branch, carbon abundance, nitrogen abundance, metal-poor globular clusters, NGC 5466, M3, M13, M92, M15, first dredge-up, chemical abundances

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