An infrared spectral match between GEMS and interstellar grains

Science

Volumn 285, Issue 5434, 1999, Pages 1716-1718

  Bradley, John P ^a,b   Keller, Lindsay P ^a   Snow, Theodore P ^c   Hanner, Martha S ^d   Flynn, George J ^e   Gezo, Joseph C ^a   Clemett, Simon J ^a   Brownlee, Donald E ^f   Bowey, Janet E ^g  

^a MVA SCIENTIFIC CONSULTANTS   (United States)

^b Georgia Institute of Technology   (United States)

^c UNIVERSITY OF COLORADO   (United States)

^d CALIFORNIA INSTITUTE OF TECHNOLOGY   (United States)

^e UNIVERSITY OF WASHINGTON   (United States)

^f STATE UNIVERSITY OF NEW YORK   (United States)

^g QUEEN MARY UNIVERSITY OF LONDON   (United Kingdom)

Author keywords

[No Author keywords available]

Indexed keywords

ARTICLE; ASTRONOMY; COSMIC RADIATION; INFRARED RADIATION; PRIORITY JOURNAL; SPECTROPHOTOMETRY;

NASA DISCIPLINE EXOBIOLOGY; NON-NASA CENTER;

COSMIC DUST; MAGNESIUM SILICATES; METEOROIDS; SILICATES; SPECTROPHOTOMETRY, INFRARED;

EID: 0033543633     PISSN: 00368075     EISSN: None     Source Type: Journal    
DOI: 10.1126/science.285.5434.1716     Document Type: Article

References (62)

1. S. A. Sandford and R. M. Walker, Astrophys. J. 291, 838 (1985); D. E. Brownlee, Annu. Rev. Earth Planet. Sci. 13, 147 (1985); S. A. Sandford, Fund. Cosmic Phys. 12, 1 (1987); S. F. Dermott et al., Nature 369, 719 (1994).
2. S. A. Sandford and R. M. Walker, Astrophys. J. 291, 838 (1985); D. E. Brownlee, Annu. Rev. Earth Planet. Sci. 13, 147 (1985); S. A. Sandford, Fund. Cosmic Phys. 12, 1 (1987); S. F. Dermott et al., Nature 369, 719 (1994).
3. S. A. Sandford and R. M. Walker, Astrophys. J. 291, 838 (1985); D. E. Brownlee, Annu. Rev. Earth Planet. Sci. 13, 147 (1985); S. A. Sandford, Fund. Cosmic Phys. 12, 1 (1987); S. F. Dermott et al., Nature 369, 719 (1994).
4. S. A. Sandford and R. M. Walker, Astrophys. J. 291, 838 (1985); D. E. Brownlee, Annu. Rev. Earth Planet. Sci. 13, 147 (1985); S. A. Sandford, Fund. Cosmic Phys. 12, 1 (1987); S. F. Dermott et al., Nature 369, 719 (1994).
5. J. P. Bradley and D. E. Brownlee, Science 231, 1542 (1986); K. L. Thomas et al., Geochim. Cosmochim. Acta 57, 1551 (1993); D. E. Brownlee et al., Lunar Planet. Sci. Conf. XXV, 185 (1994); S. A. Sandford and J. P. Bradley, Icarus 82, 146 (1989).
6. J. P. Bradley and D. E. Brownlee, Science 231, 1542 (1986); K. L. Thomas et al., Geochim. Cosmochim. Acta 57, 1551 (1993); D. E. Brownlee et al., Lunar Planet. Sci. Conf. XXV, 185 (1994); S. A. Sandford and J. P. Bradley, Icarus 82, 146 (1989).
7. J. P. Bradley and D. E. Brownlee, Science 231, 1542 (1986); K. L. Thomas et al., Geochim. Cosmochim. Acta 57, 1551 (1993); D. E. Brownlee et al., Lunar Planet. Sci. Conf. XXV, 185 (1994); S. A. Sandford and J. P. Bradley, Icarus 82, 146 (1989).
8. J. P. Bradley and D. E. Brownlee, Science 231, 1542 (1986); K. L. Thomas et al., Geochim. Cosmochim. Acta 57, 1551 (1993); D. E. Brownlee et al., Lunar Planet. Sci. Conf. XXV, 185 (1994); S. A. Sandford and J. P. Bradley, Icarus 82, 146 (1989).
9. J. P. Bradley, T. P. Snow, D. E. Brownlee, M. S. Hanner, in Solid Interstellar Matter: The ISO Revolution, L. d'Hendecourt, C. Joblin, A. Jones, Eds. (Les Houches 11, EDP Sciences, Les Ullis, France; Springer-Verlag, Berlin, 1999), pp. 298-315.
10. J. M. Greenberg, in Comets, L. L. Wilkening, Ed. (Univ. of Arizona Press, Tucson, AZ, 1982), pp. 131-163; L. B. F. M. Waters et al., Nature 391, 868 (1998).
11. J. M. Greenberg, in Comets, L. L. Wilkening, Ed. (Univ. of Arizona Press, Tucson, AZ, 1982), pp. 131-163; L. B. F. M. Waters et al., Nature 391, 868 (1998).
12. D. H. Wooden et al., Astrophys. J. 517, 1034 (1999).
13. J. Crovisier et al., Science 275, 1904 (1997).
14. J. P. Bradley, ibid. 265, 925 (1994).
15. G. J. Flynn, Nature 371, 287 (1994).
16. GEMS are glassy spheroids, 0.1 to 0.5 μm in diameter, with nanometer-sized opaque (metal and sulfide) inclusions embedded in nonstoichiometric Mg-silicate glass, and chondritic bulk compositions (Fig. 1) (7). These properties are exotic (relative to other natural silicates) but similar to those of astronomical "amorphous" silicate grains [P. G. Martin, Astrophys. J. 445, L63 (1995)]. Observations and theory suggest that the astronomical silicates are predominantly amorphous (glassy), spheroidal in shape, and "dirty" (light absorbing) because they contain opaque inclusions, some or all of which may be superparamagnetic [A. A. Goodman and D. C. B. Whittet, ibid. 455, L181 (1995)]. The size range of the grains inferred from extinction is 0.1 to 0.5 μm [S. H. Kim, P. G. Martin, P. D. Hendry, ibid. 422, 164 (1994)], and their bulk compositions inferred from interstellar gas phase abundances are about chondritic (31).
17. GEMS are glassy spheroids, 0.1 to 0.5 μm in diameter, with nanometer-sized opaque (metal and sulfide) inclusions embedded in nonstoichiometric Mg-silicate glass, and chondritic bulk compositions (Fig. 1) (7). These properties are exotic (relative to other natural silicates) but similar to those of astronomical "amorphous" silicate grains [P. G. Martin, Astrophys. J. 445, L63 (1995)]. Observations and theory suggest that the astronomical silicates are predominantly amorphous (glassy), spheroidal in shape, and "dirty" (light absorbing) because they contain opaque inclusions, some or all of which may be superparamagnetic [A. A. Goodman and D. C. B. Whittet, ibid. 455, L181 (1995)]. The size range of the grains inferred from extinction is 0.1 to 0.5 μm [S. H. Kim, P. G. Martin, P. D. Hendry, ibid. 422, 164 (1994)], and their bulk compositions inferred from interstellar gas phase abundances are about chondritic (31).
18. GEMS are glassy spheroids, 0.1 to 0.5 μm in diameter, with nanometer-sized opaque (metal and sulfide) inclusions embedded in nonstoichiometric Mg-silicate glass, and chondritic bulk compositions (Fig. 1) (7). These properties are exotic (relative to other natural silicates) but similar to those of astronomical "amorphous" silicate grains [P. G. Martin, Astrophys. J. 445, L63 (1995)]. Observations and theory suggest that the astronomical silicates are predominantly amorphous (glassy), spheroidal in shape, and "dirty" (light absorbing) because they contain opaque inclusions, some or all of which may be superparamagnetic [A. A. Goodman and D. C. B. Whittet, ibid. 455, L181 (1995)]. The size range of the grains inferred from extinction is 0.1 to 0.5 μm [S. H. Kim, P. G. Martin, P. D. Hendry, ibid. 422, 164 (1994)], and their bulk compositions inferred from interstellar gas phase abundances are about chondritic (31).
19. J. Gürtler, T. Henning, J. Dorschner, Astron. Nachr. 310, 319 (1989).
20. -1.
21. J. Reffner et al., Synch. Rad. News 7, 30 (1994); G. L. Carr, J. A. Reffner, G. P. Williams, Rev. Sci. Instrum. 66, 1490 (1995).
22. J. Reffner et al., Synch. Rad. News 7, 30 (1994); G. L. Carr, J. A. Reffner, G. P. Williams, Rev. Sci. Instrum. 66, 1490 (1995).
23. D. E. Brownlee, D. J. Joswiak, J. P. Bradley, Lunar Planet. Sci. Conf. XXX, 2031 (1999).
24. J. P. Bradley, H. Humecki, M. S. Germani, Astrophys. J. 394, 643 (1992); J. P. Bradley et al., Lunar Planet. Sci. Conf. XXIX 1737 (1998).
25. J. P. Bradley, H. Humecki, M. S. Germani, Astrophys. J. 394, 643 (1992); J. P. Bradley et al., Lunar Planet. Sci. Conf. XXIX 1737 (1998).
26. H. Campins and E. Ryan, Astrophys. J. 341, 1059 (1989).
27. M. S. Hanner et al., Earth Moon Planets, in press.
28. M. L. Sitko, C. A. Grady, D. K. Lynch, R. W. Russell, M. S. Hanner, Astrophys. J. 510, 408 (1999).
29. J. E. Bowey, A. J. Adamson, D. Whittet, Mon. Not. R. Astron. Soc. 298, 131 (1998); J. E. Bowey, thesis, University of Central Lancashire (1997).
30. J. E. Bowey, A. J. Adamson, D. Whittet, Mon. Not. R. Astron. Soc. 298, 131 (1998); J. E. Bowey, thesis, University of Central Lancashire (1997).
31. M. S. Hanner, T. Y. Brooke, A. T. Tokunaga, Astrophys. J. 438, 250 (1995).
32. M. S. Hanner, T. Y. Brooke, A. T. Tokunaga, ibid. 502, 871 (1998).
33. D. K. Aitken et al., Mon. Not. R. Astron. Soc. 230, 629 (1988).
34. J. P. Bradley et al., Lunar Planet. Sci. Conf. XXX, 1835 (1999).
35. J. P. Simpson, Astrophys. J. 368, 570 (1991); Th. Henning and R. Stognienko, Astron. Astrophys. 280, 609 (1993).
36. J. P. Simpson, Astrophys. J. 368, 570 (1991); Th. Henning and R. Stognienko, Astron. Astrophys. 280, 609 (1993).
37. J. R. Stephens and R. W. Russel, Astrophys. J. 228, 780 (1979); T. J. Millar and W. W. Duley, Mon. Not. R. Astron. Soc. 191, 641 (1980); M. Madon and G. D. Price, J. Geophys. Res. 94, 687 (1989); J. Jäger et al., Astron. Astrophys. 339, 904 (1998); J. Dorschner, B. Begemann, Th. Henning, C. Jaeger, H. Mutschke, ibid. 300, 503 (1995).
38. J. R. Stephens and R. W. Russel, Astrophys. J. 228, 780 (1979); T. J. Millar and W. W. Duley, Mon. Not. R. Astron. Soc. 191, 641 (1980); M. Madon and G. D. Price, J. Geophys. Res. 94, 687 (1989); J. Jäger et al., Astron. Astrophys. 339, 904 (1998); J. Dorschner, B. Begemann, Th. Henning, C. Jaeger, H. Mutschke, ibid. 300, 503 (1995).
39. J. R. Stephens and R. W. Russel, Astrophys. J. 228, 780 (1979); T. J. Millar and W. W. Duley, Mon. Not. R. Astron. Soc. 191, 641 (1980); M. Madon and G. D. Price, J. Geophys. Res. 94, 687 (1989); J. Jäger et al., Astron. Astrophys. 339, 904 (1998); J. Dorschner, B. Begemann, Th. Henning, C. Jaeger, H. Mutschke, ibid. 300, 503 (1995).
40. J. R. Stephens and R. W. Russel, Astrophys. J. 228, 780 (1979); T. J. Millar and W. W. Duley, Mon. Not. R. Astron. Soc. 191, 641 (1980); M. Madon and G. D. Price, J. Geophys. Res. 94, 687 (1989); J. Jäger et al., Astron. Astrophys. 339, 904 (1998); J. Dorschner, B. Begemann, Th. Henning, C. Jaeger, H. Mutschke, ibid. 300, 503 (1995).
41. J. R. Stephens and R. W. Russel, Astrophys. J. 228, 780 (1979); T. J. Millar and W. W. Duley, Mon. Not. R. Astron. Soc. 191, 641 (1980); M. Madon and G. D. Price, J. Geophys. Res. 94, 687 (1989); J. Jäger et al., Astron. Astrophys. 339, 904 (1998); J. Dorschner, B. Begemann, Th. Henning, C. Jaeger, H. Mutschke, ibid. 300, 503 (1995).
42. J. P. Bradley and T. Ireland, in Physics, Chemistry, and Dynamics of Interplanetary Dust, B. Å. S. Gustafson and M. S. Hanner, Eds. (ASP Conference Series 104, Astronomical Society of the Pacific, San Francisco, 1996), pp. 275-282.
43. S. Messenger and R. M. Walker, in Astrophysical Implications of the Laboratory Study of Presolar Materials, T. J. Bernatowicz and E. Zinner, Eds. (AIP Conference Proceedings 402, American Institute of Physics, Woodbury, NY, 1998), pp. 545-564.
44. L. P. Keller et al., Lunar Planet. Sci. Conf. XXVIII, 707 (1997).
45. F. J. Stadermann, R. M. Walker, E. Zinner, ibid. XXX, 1407 (1999).
46. J. A. Nuth, in Meteorites and the Early Solar System, J. Kerridge and M. S. Mathews, Eds. (Univ. of Arizona Press, Tucson, AZ, 1988), pp. 984-991.
47. U. J. Sofia, J. A. Cardelli, B. D. Savage, Astrophys. J. 430, 650 (1994); B. D. Savage and K. R. Sembach, Annu. Rev. Astron. Astrophys. 34, 279 (1996).
48. U. J. Sofia, J. A. Cardelli, B. D. Savage, Astrophys. J. 430, 650 (1994); B. D. Savage and K. R. Sembach, Annu. Rev. Astron. Astrophys. 34, 279 (1996).
49. T. P. Snow and A. N. Witt, Astrophys. J. 468, L65 (1996).
50. D. J. Jansen, E. F. van Dishoeck, J. H. Black, Astron. Astrophys. 282, 605 (1993).
51. L. Spitzer and E. L. Fitzpatrick, ibid. 409, 299 (1993); ibid. 445, 196 (1995).
52. L. Spitzer and E. L. Fitzpatrick, ibid. 409, 299 (1993); ibid. 445, 196 (1995).
53. K. Thiel, J. P. Bradley, R Spohr, Nucl. Tracks Rad. Meas. 15, 385 (1988); J. P. Bradley et al., Lunar Planet. Sci. Conf. XXVII, 149 (1996).
54. K. Thiel, J. P. Bradley, R Spohr, Nucl. Tracks Rad. Meas. 15, 385 (1988); J. P. Bradley et al., Lunar Planet. Sci. Conf. XXVII, 149 (1996).
55. J. D. Bregman et al., Astron. Astrophys. 187, 616 (1987); E. K. Jessberger, A. Christoforidis, J. Kissel. Nature 332, 691 (1988).
56. J. D. Bregman et al., Astron. Astrophys. 187, 616 (1987); E. K. Jessberger, A. Christoforidis, J. Kissel. Nature 332, 691 (1988).
57. L. B. F. M. Waters et al., Astron. Astrophys. 315, L361 (1996); C. Waelkens, L. B. F. M. Waters, M. S. de Graauw, ibid., p. L245; K. Malfait et al., ibid. 332, L25 (1998).
58. L. B. F. M. Waters et al., Astron. Astrophys. 315, L361 (1996); C. Waelkens, L. B. F. M. Waters, M. S. de Graauw, ibid., p. L245; K. Malfait et al., ibid. 332, L25 (1998).
59. L. B. F. M. Waters et al., Astron. Astrophys. 315, L361 (1996); C. Waelkens, L. B. F. M. Waters, M. S. de Graauw, ibid., p. L245; K. Malfait et al., ibid. 332, L25 (1998).
60. J. P. Bradley, D. R. Veblen, D. E. Brownlee, Nature 301, 473 (1983).
61. R. V. Jones and L. Spitzer, Astrophys. J. 147, 943 (1967).
62. Supported by NASA grants NAG5-4843, NAG5-7449, NAG5-7450, NAG5-7591, and NASW5035. We thank G. L. Carr, L. Miller, and G. P. Williams for developing and making available the IR facility at NSLS. We also thank D. Wooden, S. Sandford, and M. Sitko for data and advice.