Search

Your search keyword '"Tomeoka, K"' showing total 5 results
Start Over Author "Tomeoka, K" Database OAIster
5 results on '"Tomeoka, K"'

1. Mid-infrared spectra of differentiated meteorites (achondrites): Comparison with astronomical observations of dust in protoplanetary and debris disks

Author

Morlok, A., Koike, C., Tomeoka, K., Mason, A. B., Lisse, C. M., Anand, M., Grady, M. M., Morlok, A., Koike, C., Tomeoka, K., Mason, A. B., Lisse, C. M., Anand, M., and Grady, M. M.

Abstract

Mid-infrared (5 micron to 25 micron) transmission/absorption spectra of differentiated meteorites (achondrites) were measured to permit comparison with astronomical observations of dust in different stages of evolution of young stellar objects. In contrast to primitive chondrites, achondrites underwent heavy metamorphism and/or extensive melting and represent more advanced stages of planetesimal evolution. Spectra were obtained from primitive achondrites (acapulcoite, winonaite, ureilite, and brachinite) and differentiated achondrites (eucrite, diogenite, aubrite, and mesosiderite silicates). The ureilite and brachinite show spectra dominated by olivine features, and the diogenite and aubrite by pyroxene features. The acapulcoite, winonaite, eucrite, and mesosiderite silicates exhibit more complex spectra, reflecting their multi-phase bulk mineralogy. Mixtures of spectra of the primitive achondrites and differentiated achondrites in various proportions show good similarities to the spectra of the few Myr old protoplanetary disks HD104237A and V410 Anon 13. A spectrum of the differentiated mesosiderite silicates is similar to the spectra of the mature debris disks HD172555 and HD165014. A mixture of spectra of the primitive ureilite and brachinite is similar to the spectrum of the debris disk HD113766. The results raise the possibility that materials produced in the early stage of planetesimal differentiation occur in the protoplanetary and debris disks.

Published
2022
Full Text
View/download PDF

2. Mineralogy and petrology of comet 81P/wild 2 nucleus samples

Author

Zolensky, M., Zega, T., Yano, H., Wirick, S., Westphal, A., Weisberg, M., Weber, I., Warren, J., Velbel, M., Tsuchiyama, A., Tsou, P., Toppani, A., Tomioka, N., Tomeoka, K., Teslich, N., Taheri, M., Susini, J., Stroud, R., Stephan, T., Stadermann, F., Snead, C., Simon, S., Simionovici, A., See, T., Robert, F., Rietmeijer, F., Rao, W., Perronnet, M., Papanastassiou, D., Okudaira, K., Ohsumi, K., Ohnishi, I., Nakamura-Messenger, K., Nakamura, T., Mostefaoui, S., Mikouchi, T., Meibom, A., Matrajt, G., Marcus, M., Leroux, H., Lemelle, L., Le, L., Lanzirotti, A., Langenhorst, F., Krot, A., Keller, L., Kearsley, A., Joswiak, D., Jacob, D., Ishii, H., Harvey, R., Hagiya, K., Grossman, L., Grossman, J., Graham, G., Gounelle, M., Gillet, P., Genge, M., Flynn, G., Ferroir, T., Fallon, S., Ebel, D., Dai, Z., Cordier, P., Clark, B., Chi, M., Butterworth, A., Brownlee, D., Bridges, J., Brennan, S., Brearley, A., Bradley, J., Bleuet, P., Bland, Phil, Bastien, R., Zolensky, M., Zega, T., Yano, H., Wirick, S., Westphal, A., Weisberg, M., Weber, I., Warren, J., Velbel, M., Tsuchiyama, A., Tsou, P., Toppani, A., Tomioka, N., Tomeoka, K., Teslich, N., Taheri, M., Susini, J., Stroud, R., Stephan, T., Stadermann, F., Snead, C., Simon, S., Simionovici, A., See, T., Robert, F., Rietmeijer, F., Rao, W., Perronnet, M., Papanastassiou, D., Okudaira, K., Ohsumi, K., Ohnishi, I., Nakamura-Messenger, K., Nakamura, T., Mostefaoui, S., Mikouchi, T., Meibom, A., Matrajt, G., Marcus, M., Leroux, H., Lemelle, L., Le, L., Lanzirotti, A., Langenhorst, F., Krot, A., Keller, L., Kearsley, A., Joswiak, D., Jacob, D., Ishii, H., Harvey, R., Hagiya, K., Grossman, L., Grossman, J., Graham, G., Gounelle, M., Gillet, P., Genge, M., Flynn, G., Ferroir, T., Fallon, S., Ebel, D., Dai, Z., Cordier, P., Clark, B., Chi, M., Butterworth, A., Brownlee, D., Bridges, J., Brennan, S., Brearley, A., Bradley, J., Bleuet, P., Bland, Phil, and Bastien, R.

Published
2006

3. Comet 81P/Wild 2 Under a Microscope

Author

Brownlee, D., Tsou, P., Aléon, J., Alexander, C., Araki, T., Bajt, S., Baratta, G., Bastien, R., Bland, Phil, Bleuet, P., Borg, J., Bradley, J., Brearley, A., Brenker, F., Brennan, S., Bridges, J., Browning, N., Brucato, J., Bullock, E., Burchell, M., Busemann, H., Butterworth, A., Chaussidon, M., Cheuvront, A., Chi, M., Cintala, M., Clark, B., Clemett, S., Cody, G., Colangeli, L., Cooper, G., Cordier, P., Daghlian, C., Dai, Z., D’Hendecourt, L., Djouadi, Z., Dominguez, G., Duxbury, T., Dworkin, J., Ebel, D., Economou, T., Fakra, S., Fairey, S., Fallon, S., Ferrini, G., Ferroir, T., Fleckenstein, H., Floss, C., Flynn, G., Franchi, I., Fries, M., Gainsforth, Z., Gallien, J., Genge, M., Gilles, M., Gillet, P., Gilmour, J., Glavin, D., Gounelle, M., Grady, M., Graham, G., Grant, P., Green, S., Grossemy, F., Grossman, L., Grossman, J., Guan, Y., Hagiya, K., Harvey, R., Heck, P., Herzog, G., Hoppe, P., Hörz, F., Huth, J., Hutcheon, I., Ignatyev, K., Ishii, H., Ito, M., Jacob, D., Jacobsen, C., Jacobsen, S., Jones, S., Joswiak, D., Jurewicz, A., Kearsley, A., Keller, L., Khodja, H., Kilcoyne, A., Kissel, J., Krot, A., Langenhorst, F., Lanzirotti, A., Le, L., Leshin, L., Leitner, J., Lemelle, L., Leroux, H., Liu, M., Luening, K., Lyon, I., MacPherson, G., Marcus, M., Marhas, K., Marty, B., Matrajt, G., McKeegan, K., Meibom, A., Mennella, V., Messenger, K., Messenger, S., Mikouchi, T., Mostefaoui, S., Nakamura, T., Newville, M., Nittler, L., Ohnishi, I., Ohsumi, K., Okudaira, K., Papanastassiou, D., Palma, R., Palumbo, M., Pepin, R., Perkins, D., Perronnet, M., Pianetta, P., Rao, W., Rietmeijer, F., Robert, F., Rost, D., Rotundi, A., Ryan, R., Sandford, S., Schwandt, C., See, T., Schlutter, D., Sheffield-Parker, J., Simionovici, A., Simon, S., Sitnitsky, I., Snead, C., Stephan, T., Stadermann, F., Steele, A., Stroud, R., Susini, J., Sutton, S., Suzuki, Y., Taheri, M., Taylor, S., Teslich, N., Tomeoka, K., Tomioka, N., Toppani, A., Trigo-Rodríguez, J., Troadec, D., Tsuchiyama, A., Tuzzolino, A., Tyliszczak, T., Uesugi, K., Velbel, M., Vellenga, J., Vicenzi, E., Vincze, L., Warren, J., Weber, I., Weisberg, M., Westphal, A., Wirick, S., Wooden, D., Wopenka, B., Wozniakiewicz, P., Wright, I., Yabuta, H., Yano, H., Young, E., Zare, R., Zega, T., Ziegler, K., Zimmerman, L., Zinner, E., Zolensky, M., Brownlee, D., Tsou, P., Aléon, J., Alexander, C., Araki, T., Bajt, S., Baratta, G., Bastien, R., Bland, Phil, Bleuet, P., Borg, J., Bradley, J., Brearley, A., Brenker, F., Brennan, S., Bridges, J., Browning, N., Brucato, J., Bullock, E., Burchell, M., Busemann, H., Butterworth, A., Chaussidon, M., Cheuvront, A., Chi, M., Cintala, M., Clark, B., Clemett, S., Cody, G., Colangeli, L., Cooper, G., Cordier, P., Daghlian, C., Dai, Z., D’Hendecourt, L., Djouadi, Z., Dominguez, G., Duxbury, T., Dworkin, J., Ebel, D., Economou, T., Fakra, S., Fairey, S., Fallon, S., Ferrini, G., Ferroir, T., Fleckenstein, H., Floss, C., Flynn, G., Franchi, I., Fries, M., Gainsforth, Z., Gallien, J., Genge, M., Gilles, M., Gillet, P., Gilmour, J., Glavin, D., Gounelle, M., Grady, M., Graham, G., Grant, P., Green, S., Grossemy, F., Grossman, L., Grossman, J., Guan, Y., Hagiya, K., Harvey, R., Heck, P., Herzog, G., Hoppe, P., Hörz, F., Huth, J., Hutcheon, I., Ignatyev, K., Ishii, H., Ito, M., Jacob, D., Jacobsen, C., Jacobsen, S., Jones, S., Joswiak, D., Jurewicz, A., Kearsley, A., Keller, L., Khodja, H., Kilcoyne, A., Kissel, J., Krot, A., Langenhorst, F., Lanzirotti, A., Le, L., Leshin, L., Leitner, J., Lemelle, L., Leroux, H., Liu, M., Luening, K., Lyon, I., MacPherson, G., Marcus, M., Marhas, K., Marty, B., Matrajt, G., McKeegan, K., Meibom, A., Mennella, V., Messenger, K., Messenger, S., Mikouchi, T., Mostefaoui, S., Nakamura, T., Newville, M., Nittler, L., Ohnishi, I., Ohsumi, K., Okudaira, K., Papanastassiou, D., Palma, R., Palumbo, M., Pepin, R., Perkins, D., Perronnet, M., Pianetta, P., Rao, W., Rietmeijer, F., Robert, F., Rost, D., Rotundi, A., Ryan, R., Sandford, S., Schwandt, C., See, T., Schlutter, D., Sheffield-Parker, J., Simionovici, A., Simon, S., Sitnitsky, I., Snead, C., Stephan, T., Stadermann, F., Steele, A., Stroud, R., Susini, J., Sutton, S., Suzuki, Y., Taheri, M., Taylor, S., Teslich, N., Tomeoka, K., Tomioka, N., Toppani, A., Trigo-Rodríguez, J., Troadec, D., Tsuchiyama, A., Tuzzolino, A., Tyliszczak, T., Uesugi, K., Velbel, M., Vellenga, J., Vicenzi, E., Vincze, L., Warren, J., Weber, I., Weisberg, M., Westphal, A., Wirick, S., Wooden, D., Wopenka, B., Wozniakiewicz, P., Wright, I., Yabuta, H., Yano, H., Young, E., Zare, R., Zega, T., Ziegler, K., Zimmerman, L., Zinner, E., and Zolensky, M.

Published
2006

4. Mid-infrared spectra of the shocked Murchison CM chondrite: comparison with astronomical observations of dust in debris disks

Author

Morlok, A., Koike, C., Tomioka, N., Mann, I., Tomeoka, K., Morlok, A., Koike, C., Tomioka, N., Mann, I., and Tomeoka, K.

Abstract

We present laboratory mid-infrared transmission/absorption spectra obtained from matrix of the hydrated Murchison CM meteorite experimentally shocked at peak pressures of 10-49 GPa, and compare them to astronomical observations of circumstellar dust in different stages of the formation of planetary systems. The laboratory spectra of the Murchison samples exhibit characteristic changes in the infrared features. A weakly shocked sample (shocked at 10 GPa) shows almost no changes from the unshocked sample dominated by hydrous silicate (serpentine). Moderately shocked samples (21-34 GPa) have typical serpentine features gradually replaced by bands of amorphous material and olivine with increasing shock pressure. A strongly shocked sample (36 GPa) shows major changes due to decomposition of the serpentine and due to devolatilization. A shock melted sample (49 GPa) shows features of olivine recrystallized from melted material. The infrared spectra of the shocked Murchison samples show similarities to astronomical spectra of dust in various young stellar objects and debris disks. The spectra of highly shocked Murchison samples (36 and 49 GPa) are similar to those of dust in the debris disks of HD113766 and HD69830, and the transitional disk of HD100546. The moderately shocked samples (21-34 GPa) exhibit spectra similar to those of dust in the debris disks of Beta Pictoris and BD+20307, and the transitional disk of GM Aur. An average of the spectra of all Murchison samples (0-49 GPa) has a similarity to the spectrum of the older proto-planetary disk of SU Auriga. In the gas-rich transitional and protoplanetary disks, the abundances of amorphous silicates and gases have widely been considered to be a primary property. However, our study suggests that impact processing may play a significant role in generating secondary amorphous silicates and gases in those disks. Infrared spectra of the shocked Murchison samples also show similarities to the dust fromcomets (C/2002 V1, C/20

5. Mid-infrared spectra of the shocked Murchison CM chondrite: comparison with astronomical observations of dust in debris disks

Author

Morlok, A., Koike, C., Tomioka, N., Mann, I., Tomeoka, K., Morlok, A., Koike, C., Tomioka, N., Mann, I., and Tomeoka, K.

Abstract

We present laboratory mid-infrared transmission/absorption spectra obtained from matrix of the hydrated Murchison CM meteorite experimentally shocked at peak pressures of 10-49 GPa, and compare them to astronomical observations of circumstellar dust in different stages of the formation of planetary systems. The laboratory spectra of the Murchison samples exhibit characteristic changes in the infrared features. A weakly shocked sample (shocked at 10 GPa) shows almost no changes from the unshocked sample dominated by hydrous silicate (serpentine). Moderately shocked samples (21-34 GPa) have typical serpentine features gradually replaced by bands of amorphous material and olivine with increasing shock pressure. A strongly shocked sample (36 GPa) shows major changes due to decomposition of the serpentine and due to devolatilization. A shock melted sample (49 GPa) shows features of olivine recrystallized from melted material. The infrared spectra of the shocked Murchison samples show similarities to astronomical spectra of dust in various young stellar objects and debris disks. The spectra of highly shocked Murchison samples (36 and 49 GPa) are similar to those of dust in the debris disks of HD113766 and HD69830, and the transitional disk of HD100546. The moderately shocked samples (21-34 GPa) exhibit spectra similar to those of dust in the debris disks of Beta Pictoris and BD+20307, and the transitional disk of GM Aur. An average of the spectra of all Murchison samples (0-49 GPa) has a similarity to the spectrum of the older proto-planetary disk of SU Auriga. In the gas-rich transitional and protoplanetary disks, the abundances of amorphous silicates and gases have widely been considered to be a primary property. However, our study suggests that impact processing may play a significant role in generating secondary amorphous silicates and gases in those disks. Infrared spectra of the shocked Murchison samples also show similarities to the dust fromcomets (C/2002 V1, C/20

Catalog

Books, media, physical & digital resources
See catalog results