Relevant bibliographies by topics / Protoplanetary nebula

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  2. Dissertations / Theses
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Academic literature on the topic 'Protoplanetary nebula'

Author: Grafiati
Published: 4 June 2021
Last updated: 8 February 2022

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Journal articles on the topic "Protoplanetary nebula"

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Howe, D. A., T. J. Millar, and D. A. Williams. "Chemistry in a protoplanetary nebula." Monthly Notices of the Royal Astronomical Society 255, no. 2 (March 15, 1992): 217–26. http://dx.doi.org/10.1093/mnras/255.2.217.

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Weiss, Benjamin P., Xue-Ning Bai, and Roger R. Fu. "History of the solar nebula from meteorite paleomagnetism." Science Advances 7, no. 1 (January 2021): eaba5967. http://dx.doi.org/10.1126/sciadv.aba5967.

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We review recent advances in our understanding of magnetism in the solar nebula and protoplanetary disks (PPDs). We discuss the implications of theory, meteorite measurements, and astronomical observations for planetary formation and nebular evolution. Paleomagnetic measurements indicate the presence of fields of 0.54 ± 0.21 G at ~1 to 3 astronomical units (AU) from the Sun and ≳0.06 G at 3 to 7 AU until >1.22 and >2.51 million years (Ma) after solar system formation, respectively. These intensities are consistent with those predicted to enable typical astronomically observed protostellar accretion rates of ~10−8M⊙year−1, suggesting that magnetism played a central role in mass transport in PPDs. Paleomagnetic studies also indicate fields <0.006 G and <0.003 G in the inner and outer solar system by 3.94 and 4.89 Ma, respectively, consistent with the nebular gas having dispersed by this time. This is similar to the observed lifetimes of extrasolar protoplanetary disks.
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Fang, Xuan, Martín Guerrero, Ana Castro, Jesús Toalá, Bruce Balick, and Angels Riera. "UV Monochromatic Imaging of the Protoplanetary Nebula Hen 3-1475 Using HST STIS." Galaxies 6, no. 4 (December 14, 2018): 141. http://dx.doi.org/10.3390/galaxies6040141.

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Collimated outflows and jets play a critical role in shaping planetary nebulae (PNe), especially in the brief transition from a spherical AGB envelope to an aspherical PN, which is called the protoplanetary nebula (pPN) phase. We present UV observations of Hen 3-1475, a bipolar pPN with fast, highly collimated jets, obtained with STIS on board the Hubble Space Telescope (HST). The deep, low-dispersion spectroscopy enabled monochromatic imaging of Hen 3-1475 in different UV nebular emission lines; this is the first of such attempt ever conducted for a pPN. The northwest inner knot (NW1) is resolved into four components in Mg ii λ 2800. Through comparison analysis with the HST optical narrowband images obtained 6 yr earlier, we found that these components of NW1 hardly move, despite of a negative gradient of high radial velocities, from −1550 km s - 1 on the innermost component to ∼−300 km s - 1 on the outermost. These NW1 knot components might thus be quasi-stationary shocks near the tip of the conical outflow of Hen 3-1475.
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Cox, Pierre, Jean-Pierre Maillard, P. J. Huggins, T. Forveille, R. Bachiller, S. Guilloteau, and A. Omont. "K’-Band Spectro-imagery of AFGL 2688 and NGC 7027." International Astronomical Union Colloquium 149 (1995): 332–35. http://dx.doi.org/10.1017/s0252921100023265.

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Podolak, M., and Y. Mekler. "Dirty ice grains in the protoplanetary nebula." Planetary and Space Science 45, no. 11 (November 1997): 1401–6. http://dx.doi.org/10.1016/s0032-0633(97)00143-8.

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Davis, Sanford S. "Condensation Front Migration in a Protoplanetary Nebula." Astrophysical Journal 620, no. 2 (February 20, 2005): 994–1001. http://dx.doi.org/10.1086/427073.

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Dubrulle, B., G. Morfill, and M. Sterzik. "The Dust Subdisk in the Protoplanetary Nebula." Icarus 114, no. 2 (April 1995): 237–46. http://dx.doi.org/10.1006/icar.1995.1058.

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Klochkova, V. G., V. E. Panchuk, M. V. Yushkin, and A. S. Miroshnichenko. "Polarimetry of the protoplanetary nebula AFGL 2688." Astronomy Reports 48, no. 4 (April 2004): 288–300. http://dx.doi.org/10.1134/1.1704674.

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Russell, Sara S., Enrica Bonato, Helena Bates, Ashley J. King, Natasha V. Almeida, and Paul F. Schofield. "Carbonaceous chondrite meteorites as a record of protoplanetary disk conditions." Proceedings of the International Astronomical Union 15, S350 (April 2019): 135–38. http://dx.doi.org/10.1017/s1743921319009177.

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AbstractChondritic meteorites, and especially the most volatile-rich chondrites, the carbonaceous chondrites, preserve a record of the solar protoplanetary disk dust component and how it has been changed both in the disk environment itself and in its asteroidal parent body. Here we review some of the key features of carbonaceous chondrites and report some new data on their organics component. These show that the nebula reached temperature of >10000C, but only very locally, to produce chondrules. Most meteoritic material underwent thermal and/or aqueous processing, but some retain delicate nebular components such as complex organic molecules and amorphous silicates.
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Howe, D. A., T. J. Millar, and D. A. Williams. "Chemistry in Protoplanetary Nebulae." Symposium - International Astronomical Union 150 (1992): 363–64. http://dx.doi.org/10.1017/s0074180900090392.

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We have investigated gas-phase chemistry in a remnant red giant wind, during transition to a planetary nebula, using the interacting stellar winds model. Rapid destruction by UV of most existing molecules is predicted, within ~ 100 yrs of the core star heating up, suggesting that the large molecules in CRL 618 may be destroyed within decades. However, significant abundances of some hydrogenated molecules and ions (eg. CH+, CH2+, CH3+, CH, CH2, NH) may form behind the shock predicted by the interacting stellar winds model. Also, survival and/or formation of observable amounts of some molecules (eg. HCN, CN, HC3N) may occur in dense clumps which survive transition, and may explain the existence eg. of HCN in NGC 7027.
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Dissertations / Theses on the topic "Protoplanetary nebula"

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Sheehan, Patrick D., Josh A. Eisner, Rita K. Mann, and Jonathan P. Williams. "A VLA SURVEY FOR FAINT COMPACT RADIO SOURCES IN THE ORION NEBULA CLUSTER." IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/622165.

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We present Karl G. Jansky Very Large Array 1.3, 3.6, and 6 cm continuum maps of compact radio sources in the Orion Nebular Cluster (ONC). We mosaicked 34 arcmin(2) at 1.3 cm, 70 arcmin(2) at 3.6 cm and 109 arcmin(2) at 6 cm, containing 778 near-infrared detected young stellar objects and 190 Hubble Space Telescope-identified proplyds (with significant overlap between those characterizations). We detected radio emission from 175 compact radio sources in the ONC, including 26 sources that were detected for the first time at these wavelengths. For each detected source, we fitted a simple free-free and dust emission model to characterize the radio emission. We extrapolate the free-free emission spectrum model for each source to ALMA bands to illustrate how these measurements could be used to correctly measure protoplanetary disk dust masses from submillimeter flux measurements. Finally, we compare the fluxes measured in this survey with previously measured fluxes for our targets, as well as four separate epochs of 1.3 cm data, to search for and quantify the variability of our sources.
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Wu, Ya-Lin, Laird M. Close, Jinyoung Serena Kim, Jared R. Males, and Katie M. Morzinski. "The Intricate Structure of HH 508, the Brightest Microjet in the Orion Nebula." IOP PUBLISHING LTD, 2018. http://hdl.handle.net/10150/627097.

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We present Magellan adaptive optics Ha imaging of HH 508, which has the highest surface brightness among protostellar jets in the Orion Nebula. We find that HH 508 actually has a shorter component to the west, and a longer and knotty component to the east. The east component has a kink at 0.'' 3 from the jet-driving star theta(1) Ori B-2, so it may have been deflected by the wind/radiation from the nearby theta(1) Ori B1B5. The origin of both components is unclear, but if each of them is a separate jet, then theta(1) Ori B-2 may be a tight binary. Alternatively, HH 508 may be a slow-moving outflow, and each component represents an illuminated cavity wall. The ionization front surrounding theta(1) Ori B2B3 does not directly face theta(1) Ori B1B5, suggesting that the EUV radiation from theta(1) Ori C plays a dominant role in affecting the morphology of proplyds even in the vicinity of theta(1) Ori B1B5. Finally, we report an Ha blob that might be ejected by the binary proplyd LV 1.
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Dvořáková, Nela. "Spektrální diagnostika látky v okolí ranných hvězd." Master's thesis, 2019. http://www.nusl.cz/ntk/nusl-405269.

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Nela Dvořáková 19.7.2019 1 Abstract We study a representative of a diverse group of stars exhibiting the B[e] phe- nomenon, designated MWC 939. This object might be an important link be- tween the stage of the asymptotic giant branch and planetary nebula stage as it is one of a few such objects observed. Our focus is aimed at spectral analysis of the circumstellar matter around the central star. We assemble a line list for MWC 939 and observe variations of its spectrum. Electron density and temper- ature are estimated using nebular diagnostics of ratios of [S II] λλ 6716, 6731 ˚A and [O I] λλ 6300, 6364 ˚A and 5577 ˚A. These estimates are then used for detailed calculations of the structure of circumstellar envelope. 1
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渡邊, 誠一郎. "乱流太陽系星雲でのダストの生長と微惑星の形成." 1996. http://hdl.handle.net/2237/13041.

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Books on the topic "Protoplanetary nebula"

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R, Dobrovolskis Anthony, Cuzzi Jeffrey N, and United States. National Aeronautics and Space Administration., eds. A numerical turbulence model for multiphase flows in the protoplanetary nebula. [Washington, DC: National Aeronautics and Space Administration, 1995.

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R, Dobrovolskis Anthony, Cuzzi Jeff, and United States. National Aeronautics and Space Administration., eds. A numerical turbulence model for multiphase flows in the protoplanetary nebula. [Washington, DC: National Aeronautics and Space Administration, 1995.

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Book chapters on the topic "Protoplanetary nebula"

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Kwok, Sun. "Protoplanetary Nebula." In Encyclopedia of Astrobiology, 1–3. Berlin, Heidelberg: Springer Berlin Heidelberg, 2014. http://dx.doi.org/10.1007/978-3-642-27833-4_5114-7.

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Kwok, Sun. "Protoplanetary Nebula." In Encyclopedia of Astrobiology, 2073–75. Berlin, Heidelberg: Springer Berlin Heidelberg, 2015. http://dx.doi.org/10.1007/978-3-662-44185-5_5114.

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Waelkens, C. L., and L. B. F. M. Waters. "How Unique is the Protoplanetary Nebula Star HR 4049?" In Circumstellar Matter, 509–10. Dordrecht: Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-3887-8_135.

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Smith, M. G., T. R. Geballe, G. Sandell, and C. Aspin. "Hot Molecular Gas in the Protoplanetary Nebula CRL 2688." In Submillimetre Astronomy, 29–30. Dordrecht: Springer Netherlands, 1990. http://dx.doi.org/10.1007/978-94-015-6850-0_7.

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Rodríguez, Luis F. "Protoplanetary Nebulae." In Planetary and Proto-Planetary Nebulae: From IRAS to ISO, 55–67. Dordrecht: Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-3891-5_7.

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Howe, D. A., T. J. Millar, and D. A. Williams. "Chemistry in Protoplanetary Nebulae." In Astrochemistry of Cosmic Phenomena, 363–64. Dordrecht: Springer Netherlands, 1992. http://dx.doi.org/10.1007/978-94-011-2761-5_84.

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Volk, Kevin, Sun Kwok, Bruce Hrivnak, and Ryszard Szczerba. "ISO Results for Protoplanetary Nebulae." In Post-AGB Objects as a Phase of Stellar Evolution, 323–28. Dordrecht: Springer Netherlands, 2001. http://dx.doi.org/10.1007/978-94-015-9688-6_51.

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Weintraub, David A., Joel H. Kastner, and Ian Gatley. "H2 Spectroscopy of Protoplanetary Nebulae." In Post-AGB Objects as a Phase of Stellar Evolution, 377–82. Dordrecht: Springer Netherlands, 2001. http://dx.doi.org/10.1007/978-94-015-9688-6_59.

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Sahade, J., R. M. West, and M. Yu Skulskij. "A Spectrographic Study of the Interacting Eclipsing Binary RY Scuti: An Episode in the Rapid Mass Loss Stage or a Protoplanetary Nebula ?" In Evolutionary Processes in Interacting Binary Stars, 325–26. Dordrecht: Springer Netherlands, 1992. http://dx.doi.org/10.1007/978-94-011-2542-0_40.

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Pascoli, G. "Some Hypothesized Observational Aspects of Magnetic Fields in Protoplanetary Nebulae." In Planetary Nebulae, 455. Dordrecht: Springer Netherlands, 1989. http://dx.doi.org/10.1007/978-94-009-0865-9_153.

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