Relevant bibliographies by topics / Galactis bulge

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  1. Journal articles
  2. Dissertations / Theses
  3. Books
  4. Book chapters
  5. Conference papers
  6. Reports

Academic literature on the topic 'Galactis bulge'

Author: Grafiati
Published: 4 June 2021
Last updated: 9 February 2022

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Journal articles on the topic "Galactis bulge"

1

Freeman, K. C. "Galactic bulges: overview." Proceedings of the International Astronomical Union 3, S245 (July 2007): 3–10. http://dx.doi.org/10.1017/s1743921308017146.

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AbstractThis overview of galactic bulges begins with a discussion of the various kinds of bulges (classical, boxy/peanut-shaped, pseudo) and their likely formation mechanisms. Other specific topics include the Galactic bar/bulge and its chemical evolution, the bulge of M31, the relation between bulges and metal-poor halos (often lumped together as spheroids), the morphology-density relation and the formation of S0 galaxies, the color-structure bimodality, and scaling laws for bulges. Finally I will briefly discuss the current difficulty of forming bulgeless disk galaxies in ΛCDM.
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Renzini, Alvio. "Formation and evolution of stars in galactic bulges." Symposium - International Astronomical Union 153 (1993): 151–68. http://dx.doi.org/10.1017/s0074180900123174.

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A fair fraction of stars in the Galactic Bulge (a possibly in bulges in general) appears to be more metal rich than the sun. Some of the current limitations in quantitatively modelling such super metal rich (SMR) stars are briefly recalled, including the question of the helium enrichment, of the metallicity dependence of mass loss, and of the metal opacity. Recent color-magnitude diagrams for stars in the Galactic Bulge are show that the bulk of Bulge stars must be very old, although current data do not allow to determine the age with sufficient accuracy to establish the relative age of the Halo and of the Bulge. The question of the nature of the most luminous (AGB) stars in bulges and in M32 is then addressed in some detail, discussing a series of methodological aspects which would need careful consideration before using bright AGB stars as age indicators. It is concluded that — for the time being — none of the claims for the presence of an intermediate age component in the Galactic Bulge, in M32, and in the bulge of M31 is completely exempt from ambiguities, and ways for elimitating such ambiguities are suggested. Finally, from the evidence that bulges are dominated by a very old stellar population it is concluded that star formation in bulges probably started and was essentially completed before the completion of star formation in the halo: bulges are likely to on average older than halos.
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Arimoto, N. "Stellar population synthesis: Application To Galactic Bulges." Symposium - International Astronomical Union 153 (1993): 133–50. http://dx.doi.org/10.1017/s0074180900123162.

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The stellar populations give traces of the formation history of the bulges. The metallicity distribution of K-giants in the Galactic bulge resembles to that of the giant ellipticals. There seems to be no conspicuous colour-magnitude relation intrinsic to the bulges. This can be explained if the bulges formed by the dissipative collapse of central regions of proto-galaxies followed by the supernova-driven bulge wind which was induced later than the dwarf ellipticals of the similar mass (the biased wind). Unfortunately, the observational data available at present of stellar populations of the bulges are not yet sufficient to get a firm conclusion on the origin of the bulges.
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Breda, Iris, and Polychronis Papaderos. "The continuous rise of bulges out of galactic disks." Astronomy & Astrophysics 614 (June 2018): A48. http://dx.doi.org/10.1051/0004-6361/201731705.

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Context. A key subject in extragalactic astronomy concerns the chronology and driving mechanisms of bulge formation in late-type galaxies (LTGs). The standard scenario distinguishes between classical bulges and pseudo-bulges (CBs and PBs, respectively), the first thought to form monolithically prior to disks and the second gradually out of disks. These two bulge formation routes obviously yield antipodal predictions on the bulge age and bulge-to-disk age contrast, both expected to be high (low) in CBs (PBs). Aims. Our main goal is to explore whether bulges in present-day LTGs segregate into two evolutionary distinct classes, as expected from the standard scenario. Other questions motivating this study center on evolutionary relations between LTG bulges and their hosting disks, and the occurrence of accretion-powered nuclear activity as a function of bulge stellar mass ℳ⋆ and stellar surface density Σ⋆. Methods. In this study, we have combined three techniques – surface photometry, spectral modeling of integral field spectroscopy data and suppression of stellar populations younger than an adjustable age cutoff with the code REMOVEYOUNG (ℛ𝒴) – toward a systematic analysis of the physical and evolutionary properties (e.g., ℳ⋆, Σ⋆ and mass-weighted stellar age 〈t⋆〉ℳ and metallicity 〈Z⋆〉ℳ, respectively) of a representative sample of 135 nearby (≤ 130 Mpc) LTGs from the CALIFA survey that cover a range between 108.9 M⊙ and 1011.5 M⊙ in total stellar mass ℳ⋆,T. In particular, the analysis here revolves around ⟨δμ9G⟩, a new distance- and formally extinction-independent measure of the contribution by stellar populations of age ≥ 9 Gyr to the mean r-band surface brightness of the bulge. We argue that ⟨δμ9G⟩ offers a handy semi-empirical tracer of the physical and evolutionary properties of LTG bulges and a promising means for their characterization. Results. The essential insight from this study is that LTG bulges form over 3 dex in ℳ⋆ and more than 1 dex in Σ⋆ a tight continuous sequence of increasing ⟨δμ9G⟩ with increasing ℳ⋆, Σ⋆, 〈t⋆〉ℳ and 〈Z⋆〉ℳ. Along this continuum of physical and evolutionary properties, our sample spans a range of ~ 4 mag in ⟨δμ9G⟩: high-⟨δμ9G⟩ bulges are the oldest, densest and most massive ones (〈t⋆〉ℳ ~ 11.7 Gyr, Σ⋆ > 109 M⊙ kpc−2, ℳ⋆ ≥ 1010 M⊙), whereas the opposite is the case for low-⟨δμ9G⟩ bulges (〈t⋆〉ℳ ~ 7 Gyr) that generally reside in low-mass LTGs. Furthermore, we find that the bulge-to-disk age and metallicity contrast, as well as the bulge-to-disk mass ratio, show a positive trend with ℳ⋆,T, raising from, respectively, ~ 0 Gyr, ~ 0 dex and 0.25 to ~ 3 Gyr, ~ 0.3 dex and 0.67 across the mass range covered by our sample. Whereas gas excitation in lower-mass (≲ 109.7 M⊙) bulges is invariably dominated by star formation (SF), LINER- and Seyfert-specific emission-line ratios were exclusively documented in high-mass (≳ 1010 M⊙), high-Σ⋆ (≳ 109 M⊙ kpc−2) bulges. This is in agreement with previous work and consistent with the notion that the Eddington ratio or the black hole-to-bulge mass ratio scale with ℳ⋆. The coexistence of Seyfert and SF activity in ~20% of higher-ℳ⋆, high-Σ⋆ bulges being spectroscopically classified as Composites suggests that the onset of AGN-driven feedback does not necessarily lead to an abrupt termination of SF in LTG nuclei. Conclusions. The continuity both in the properties of LTG bulges themselves and in their age and metallicity contrast to their parent diskssuggests that these components evolve alongside in a concurrent process that leads to a continuum of physical and evolutionary characteristics. Our results are consistent with a picture where bulge growth in LTGs is driven by a superposition of quick-early and slow-secular processes, the relative importance of which increases with ℳ⋆,T. These processes, which presumably combine in situ SF in the bulge and inward migration of material from the disk, are expected to lead to a non-homologous radial growth of Σ⋆ and a trend for an increasing Sérsic index with increasing galaxy mass.
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Rich, R. Michael. "The Stellar Population of the Galactic Bulge." Symposium - International Astronomical Union 171 (1996): 19–22. http://dx.doi.org/10.1017/s0074180900232105.

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How old is the bulge? Are bulges in general as old as halos? Do bulges form rapidly or slowly? Are they formed from disks via dynamical instabilities, or perhaps by starbursts? In general, do luminous spheroids form at the same time as the oldest stars?
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Barbuy, Beatriz, Cristina Chiappini, and Ortwin Gerhard. "Chemodynamical History of the Galactic Bulge." Annual Review of Astronomy and Astrophysics 56, no. 1 (September 14, 2018): 223–76. http://dx.doi.org/10.1146/annurev-astro-081817-051826.

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The Galactic Bulge can uniquely be studied from large samples of individual stars and is therefore of prime importance for understanding the stellar population structure of bulges in general. Here the observational evidence on the kinematics, chemical composition, and ages of Bulge stellar populations based on photometric and spectroscopic data is reviewed. The bulk of Bulge stars are old and span a metallicity range of −1.5≲[Fe/H]≲+0.5. Stellar populations and chemical properties suggest a star-formation timescale below ∼2 Gyr. The overall Bulge is barred and follows cylindrical rotation, and the more metal-rich stars trace a box/peanut (B/P) structure. Dyna-mical models demonstrate the different spatial and orbital distributions of metal-rich and metal-poor stars. We discuss current Bulge-formation scenarios based on dynamical, chemical, chemodynamical, and cosmological models. Despite impressive progress, we do not yet have a successful fully self-consistent chemodynamical Bulge model in the cosmological framework, and we will also need a more extensive chrono-chemical-kinematic 3D map of stars to better constrain such models.
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Martinez-Valpuesta, Inma, and E. Athanassoula. "Boxy/peanut bulges, vertical buckling and galactic bars." Proceedings of the International Astronomical Union 3, S245 (July 2007): 103–6. http://dx.doi.org/10.1017/s1743921308017390.

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AbstractBoxy/peanut bulges in disk galaxies have been associated to stellar bars. In this talk, we discuss the different properties of such bulges and their relation with the corresponding bar, using a very large sample of a few hundred numerical N-body simulations. We present and inter-compare various methods of measuring the boxy/peanut bulge properties, namely its strength, shape and possible asymmetry. Some of these methods can be applied to both simulations and observations. Our final goal is to get correlations that will allow us to obtain information on the boxy/peanut bulge for a galaxy viewed face-on as well as information on the bars of galaxies viewed edge-on.
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Ballero, Silvia K., Francesca Matteucci, and Luca Ciotti. "Chemical evolution of Seyfert galaxies." Proceedings of the International Astronomical Union 3, S245 (July 2007): 231–32. http://dx.doi.org/10.1017/s1743921308017729.

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AbstractWe computed the chemical evolution of Seyfert galaxies, residing in spiral bulges, based on an updated model for the Milky Way bulge with updated calculations of the Galactic potential and of the feedback from the central supermassive black hole (BH) in a spherical approximation. We followed the evolution of bulges of masses 2 × 109 − 1011M⊙ by scaling the star-formation efficiency and the bulge scalelenght as in the inverse-wind scenario for ellipticals. We successfully reproduced the observed relation between the BH mass and that of the host bulge, and the observed peak nuclear bolometric luminosity. The observed metal overabundances are easily achieved, as well as the constancy of chemical abundances with the redshift.
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Gargiulo, Ignacio D., Antonela Monachesi, Facundo A. Gómez, Robert J. J. Grand, Federico Marinacci, Rüdiger Pakmor, Simon D. M. White, Eric F. Bell, Francesca Fragkoudi, and Patricia Tissera. "The prevalence of pseudo-bulges in the Auriga simulations." Monthly Notices of the Royal Astronomical Society 489, no. 4 (September 11, 2019): 5742–63. http://dx.doi.org/10.1093/mnras/stz2536.

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ABSTRACT We study the galactic bulges in the Auriga simulations, a suite of 30 cosmological magneto-hydrodynamical zoom-in simulations of late-type galaxies in Milky Way sized dark matter haloes performed with the moving-mesh code arepo. We aim to characterize bulge formation mechanisms in this large suite of galaxies simulated at high resolution in a fully cosmological context. The bulges of the Auriga galaxies show a large variety in their shapes, sizes, and formation histories. According to observational classification criteria, such as Sérsic index and degree of ordered rotation, the majority of the Auriga bulges can be classified as pseudo-bulges, while some of them can be seen as composite bulges with a classical component; however, none can be classified as a classical bulge. Auriga bulges show mostly an in situ origin, $21{{\ \rm per\ cent}}$ of them with a negligible accreted fraction (facc < 0.01). In general, their in situ component was centrally formed, with ${\sim}75{{\ \rm per\ cent}}$ of the bulges forming most of their stars inside the bulge region at z = 0. Part of their in situ mass growth is rapid and is associated with the effects of mergers, while another part is more secular in origin. In $90{{\ \rm per\ cent}}$ of the Auriga bulges, the accreted bulge component originates from less than four satellites. We investigate the relation between the accreted stellar haloes and the bulges of the Auriga simulations. The total bulge mass shows no correlation with the accreted stellar halo mass, as in observations. However, the accreted mass of bulges tends to correlate with their respective accreted stellar halo mass.
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MacArthur, Lauren A., Richard S. Ellis, and Tommaso Treu. "The fundamental plane of bulges at intermediate redshift." Proceedings of the International Astronomical Union 3, S245 (July 2007): 443–46. http://dx.doi.org/10.1017/s1743921308018322.

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AbstractWe report on a new study aimed at understanding the diversity and evolutionary properties of distant galactic bulges in the context of well-established trends for pure spheroidal galaxies. Bulges have been isolated for a sample of 137 spiral galaxies in the GOODS fields within the redshift range 0.1 < z < 1.2. Using proven photometric techniques we determine for each galaxy the characteristic parameters (size, surface brightness, profile shape) in the 4 GOODS-ACS imaging bands of both the disk and bulge components. Using the DEIMOS spectrograph on Keck, precision stellar velocity dispersions were secured for a sizeable fraction of the bulges. This has enabled us to compare the Fundamental Plane of our distant bulges with that of field spheroidal galaxies in a similar redshift range. Bulges in spiral galaxies with a bulge-to-total luminosity ratio (B/T) > 0.2 show very similar patterns of evolution to those seen for low luminosity spheroidals. To first order, their recent mass assembly histories are equivalent.
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Dissertations / Theses on the topic "Galactis bulge"

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Nataf, David M. "The Galactic Bulge Stellar Population." The Ohio State University, 2012. http://rave.ohiolink.edu/etdc/view?acc_num=osu1343225619.

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Peyaud, Alan. "The galactic bulge traced by planetary nebulae." Université Louis Pasteur (Strasbourg) (1971-2008), 2005. http://www.theses.fr/2005STR13185.

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Minniti, Dante. "Kinematics and stellar populations of the galactic bulge." Diss., The University of Arizona, 1993. http://hdl.handle.net/10150/186488.

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In order to measure radial and/or rotation velocities and obtain metallicities for the stellar population of the Galactic bulge, several hundred spectra of giants have been obtained. These include three bulge fields at projected distances from the Galactic center of 1.5, 1.7 and 1.7 kpc, and 33 globular and open clusters. We measure metallicities based on a calibration from stars belonging to the field and to clusters of known abundances. There is a clear dependence of the kinematics on metallicity in all the fields studied, in the sense that the more metal poor stars have lower rotation and higher velocity dispersion than the more metal rich stars. In particular, we identify the giants having [Fe/H] ≤ 1.0 with an extension of the halo population to the innermost regions of the Galaxy rather than with the bulge itself. Near-IR photometry of 21 globulars clusters and bulge fields within 3 kpc of the Galactic center has also been obtained. We find a metallicity gradient with radial distance from the center, consistent with previous results obtained from optical photometry. We argue that the majority of the metal rich globulars within 3 kpc of the center are associated with the bulge population. We also argue that the RR Lyraes previously studied in bulge fields are associated with the inner halo, and that the bulge is younger than the halo. Other kinematic tracers are examined (M giants, RR Lyraes, Miras, OH/IR stars, planetary nebulae) to associate them with different Galactic components. We conclude that all the existing evidence shows that dissipation played an important role in the formation of the bulge.
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Busso, Giorgia [Verfasser]. "The UV spectrum of the galactic bulge / Giorgia Busso." Kiel : Universitätsbibliothek Kiel, 2008. http://d-nb.info/1019669756/34.

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Ramírez, Santana Solange V. "Stellar abundances in the inner bulge and galactic center /." The Ohio State University, 2000. http://rave.ohiolink.edu/etdc/view?acc_num=osu1488196234909106.

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Harding, Paul. "The formation of the Galactic bulge and halo: Observational signatures." Diss., The University of Arizona, 2001. http://hdl.handle.net/10150/289743.

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The evolution of tidal debris within the Galactic halo has been simulated to determine its detectability within the constraints imposed by currently available telescopes and instrumentation. Observations of the simulations show that there is a very high probability of detecting and quantifying the presence of tidal debris with a pencil beam survey of 100 square degrees. The debris is readily detectable via the presence of kinematic substructure in the radial velocities. The detection probabilities show surprisingly little change with the age of the debris. Accretion events that occurred up to ≳ 10 Gyr ago can be detected. In the limiting case of a single 10⁷ M(⊙) satellite contributing 1% of the luminous halo mass the detection probability is a few percent using just the velocities of 100 halo stars in a single 1 deg² field. The detection probabilities scale with the accreted fraction of the halo and the number of fields surveyed. Accurate CMDs in the Washington photometric system have been derived for four fields spanning the range of Galactocentric distances from 1.5 to 5.5 kpc. The differential reddening variations within each field were corrected by a new technique optimized for the highly variable reddening variations found in bulge fields. Abundance distributions in the four fields were derived from color-color diagrams in the Washington system. The quality of the photometry which yields photometric abundances with σ[Fe/H] ≲ 0.25 dex (including reddening errors) supplemented by the luminosity information from observations in the 51 filter allows contamination by foreground and background stars to be eliminated from the bulge sample. A clear abundance gradient is seen which is consistent with the change in morphology of the CMDs. The abundance gradient is predominantly due to a decrease in the fraction of stars in the metal-rich shoulder of the abundance distributions. The modal abundance changes little. Relative to Baade's window the magnitude distribution of clump stars in the L354 B-06 field implies a bar angle of ≃ 40 deg.
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Shafi, Nebiha Bedru. "A HI search for galaxies hidden by the Galactic bulge." Master's thesis, University of Cape Town, 2008. http://hdl.handle.net/11427/4407.

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Includes abstract.
Includes bibliographical references (leaves 96-99).
In this thesis, a deep neutral hydrogen (HI) galaxy search for galaxies hidden by the Galactic Bulge is presented. The HI Parkes deep HI Zone of Avoidance (ZOA) survey has been extended towards the higher latitudes in the Galactic Bulge region. The surveyed region covers 332° ≤ l ≤ 36° for the region 5° ≤ │b│ ≤ 10° and 352° ≤ l ≤ 24° for the region 10° ≤ │b│ ≤ 15°.
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Rich, Robert Michael Mould Jeremy. "Abundances and kinematics of k giants in the galactic nuclear bulge /." Diss., Pasadena, Calif. : California Institute of Technology, 1986. http://resolver.caltech.edu/CaltechETD:etd-09102008-152942.

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Rees, Bryan. "A study of planetary nebulae in and towards the Galactic Bulge." Thesis, University of Manchester, 2011. https://www.research.manchester.ac.uk/portal/en/theses/a-study-of-planetary-nebulae-in-and-towards-the-galactic-bulge(ff6c0373-e5a5-491f-b5fb-bda36acac8ba).html.

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A planetary nebula (PN) consists of material, mainly gas, that has been ejected from a star on the asymptotic giant branch of its life cycle. This material emits electromagnetic radiation due to photoionization and recombination, collisional and radiative excitation or free-free radiation. The envelope of material moves outwards from the central star and may take one of a variety of shapes. These shapes are believed to be sculpted by the stellar wind, magnetic fields and interactions with a binary companion. However, within a time scale of as little as 10 000 years the nebula fades from view and merges with the interstellar medium.Similar variations in the shape of planetary nebulae (PNe) can be seen in both the Galactic Bulge and Disc and in the Magellanic Clouds. It is therefore reasonable to assume that the shaping process is universal. By classifying PNe by morphology and relating those shapes to other nebular properties we have attempted to derive information about that shaping process.We have used photometric narrowband observations of a sample of PNe listed in the Strasbourg-ESO Catalogue of Galactic Planetary Nebulae to investigate the relationship between PN morphology and the other PN characteristics. The high resolution images were made using ESO's New Technology Telescope and the Hubble Space Telescope. The information we could obtain directly from the observations was augmented by information in the literature in order to address that question. The observations were used to classify the morphologies of 154 PNe, to estimate the sizes of 138 of those nebulae that we considered to lie within the Galactic Bulge, to determine the orientations of 130 of those Bulge nebulae and to derive photometric fluxes for the 69 PNe which had observations of standard stars made during the same night. Information on central star binarity, nebular abundances and radial and expansion velocity was obtained from the literature.Our photometrically derived PNe line fluxes were used to verify 59 H-beta and 69 [OIII] catalogued values (which were obtained using spectroscopy). We found sufficient discrepancy between the values for 9 PNe to merit a further check taking place.We found no distinguishing relationship between PN morphology and any of PN size, radial velocity, or angular location within the Bulge. The abundances of He and O, and the N/O ratio, are generally lower in bipolar nebulae than in those nebulae with no apparent internal structure. We are unable to come to any conclusion as to a relationship between PN morphology and stellar metallicity.Given the short lifespan of PNe and the age of the Bulge it appears that almost all PNe in the Bulge must be associated with low mass stars. The high ratio of bipolar PNe we found in our Bulge sample suggests that, at least within the Bulge, bipolar nebulae are not necessarily associated with high mass stars. Our results show that unlike the orientations of other types of PNe the orientations of the bipolar nebulae in the Bulge are not randomly distributed. Measured to a line tip to tip along the lobes they peak and have their mean approximately along the Galactic Plane. This suggests that the bipolar PNe originate in a different environment from other morphological types, perhaps related to binary separation. However, we find that bipolarity does not imply common-envelope evolution. If the hypothesis that bipolar nebulae are formed in binary star systems is correct, binary systems in the Galactic Bulge have angular momentum vectors that are preferentially aligned along the Galactic Plane. As the orientation appears to be unrelated to lobe size and hence nebular age, the alignment implies that the non-random nature of the angular momentum vectors originated at the time the Bulge stellar population formed. We suggest that it is due to the direction and strength of the ambient magnetic fields.
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Houdashelt, Mark Lee. "The cool stellar populations of early-type galaxies and the Galactic bulge /." The Ohio State University, 1995. http://rave.ohiolink.edu/etdc/view?acc_num=osu1487863429095971.

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Books on the topic "Galactis bulge"

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Dejonghe, Herwig, and Harm J. Habing, eds. Galactic Bulges. Dordrecht: Springer Netherlands, 1993. http://dx.doi.org/10.1007/978-94-011-0922-2.

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Laurikainen, Eija, Reynier Peletier, and Dimitri Gadotti, eds. Galactic Bulges. Cham: Springer International Publishing, 2016. http://dx.doi.org/10.1007/978-3-319-19378-6.

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J, Jarvis B., Terndrup D. M, European Southern Observatory, and Cerro Tololo Inter-American Observatory, eds. ESO/CTIO Workshop on Bulges of Galaxies, La Serena, Chile, 16-19 January 1990: Proceedings. Garching bei München, Federal Republic of Germany: European Southern Obervatory, 1990.

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Herwig, Dejonghe, and Habing H. J. 1937-, eds. Galactic bulges: Proceedings of the 153rd Symposium of the International Astronomical Union held in Ghent, Belgium, August 17-22, 1992. Dordrecht: Kluwer Academic, 1993.

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Symposium, International Astronomical Union. Formation and evolution of galaxy bulges: Proceedings of the 245th Symposium of the International Astronomical Union, held in Oxford, United Kingdom, July 16-20, 2007. Cambridge, U.K: Cambridge University Press, 2008.

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Patterson, Timothy Graham. A survey of the Galactic Bulge,Large Magellanic Cloud and Cygnus region with a simple configuration coded mask X-ray telescope. Birmingham: University of Birmingham, 1990.

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Habing, Harm J., and Herwig Dejonghe. Galactic Bulges. Springer, 2014.

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Laurikainen, Eija, Reynier Peletier, and Dimitri Gadotti. Galactic Bulges. Springer, 2015.

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Carollo, C. Marcella, Henry C. Ferguson, and Rosemary F. G. Wyse, eds. The Formation of Galactic Bulges. Cambridge University Press, 2000. http://dx.doi.org/10.1017/cbo9780511564611.

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Galactic Bulges (International Astronomical Union Symposia). Springer, 1993.

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Book chapters on the topic "Galactis bulge"

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Freeman, Ken C. "The Galactic Bulge." In Lessons from the Local Group, 31–41. Cham: Springer International Publishing, 2014. http://dx.doi.org/10.1007/978-3-319-10614-4_3.

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Rich, R. Michael. "The Galactic Bulge." In Planets, Stars and Stellar Systems, 271–346. Dordrecht: Springer Netherlands, 2013. http://dx.doi.org/10.1007/978-94-007-5612-0_6.

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Hernandez-Pajares, M., R. Cubarsi, J. Sanz-Subirana, and J. M. Juan-Zornoza. "Detectability of Bulge Stars." In Galactic Bulges, 299–300. Dordrecht: Springer Netherlands, 1993. http://dx.doi.org/10.1007/978-94-011-0922-2_27.

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Rich, R. Michael. "The Stellar Population of the Inner 200 Parsecs." In Galactic Bulges, 169–90. Dordrecht: Springer Netherlands, 1993. http://dx.doi.org/10.1007/978-94-011-0922-2_11.

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Milone, A., and B. Barbuy. "TiO Bands in Composite Systems." In Galactic Bulges, 313–14. Dordrecht: Springer Netherlands, 1993. http://dx.doi.org/10.1007/978-94-011-0922-2_32.

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Hunter, C., and E. Qian. "Two-integral distribution functions for axisymmetric galaxies." In Galactic Bulges, 357–58. Dordrecht: Springer Netherlands, 1993. http://dx.doi.org/10.1007/978-94-011-0922-2_52.

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de Zeeuw, Tim. "Dynamics of the Galactic Bulge." In Galactic Bulges, 191–208. Dordrecht: Springer Netherlands, 1993. http://dx.doi.org/10.1007/978-94-011-0922-2_12.

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Arnold, Richard, Tim de Zeeuw, and Chris Hunter. "Kinematic signatures of triaxial stellar systems." In Galactic Bulges, 407–8. Dordrecht: Springer Netherlands, 1993. http://dx.doi.org/10.1007/978-94-011-0922-2_74.

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Balcells, Marc, and R. F. Peletier. "Colour Gradients in Galaxy Bulges." In Galactic Bulges, 409–10. Dordrecht: Springer Netherlands, 1993. http://dx.doi.org/10.1007/978-94-011-0922-2_75.

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de Souza, R. E., S. dos Anjos, and B. Barbuy. "Velocity Dispersions and Metallicities of Box-Shaped Galaxies." In Galactic Bulges, 411–12. Dordrecht: Springer Netherlands, 1993. http://dx.doi.org/10.1007/978-94-011-0922-2_76.

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Conference papers on the topic "Galactis bulge"

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Binney, James, and Ortwin Gerhard. "Dynamics of the galactic bulge-bar." In Back to the Galaxy. AIP, 1992. http://dx.doi.org/10.1063/1.43925.

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Weiland, J. L., M. G. Hauser, T. Kelsall, E. Dwek, S. H. Moseley, R. F. Silverberg, M. Mitra, et al. "Dirbe observations of the Galactic bulge." In Back to the Galaxy. AIP, 1992. http://dx.doi.org/10.1063/1.44023.

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Kuulkers, E. "The INTEGRAL Galactic Bulge monitoring program." In THE TRANSIENT MILKY WAY: A PERSPECTIVE FOR MIRAX. AIP, 2006. http://dx.doi.org/10.1063/1.2216598.

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Gnedin, Nickolay Y., Michael L. Norman, and Jeremiah P. Ostriker. "Formation of galactic bulges." In AFTER THE DARK AGES. ASCE, 1999. http://dx.doi.org/10.1063/1.58634.

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Rothschild, Richard E., William A. Heindl, John A. Tomsick, James L. Matteson, Joao Braga, Ruediger Staubert, Eckhard Kendziorra, Ronald A. Remillard, John Heise, and Jean J. M. in 't Zand. "MIRAX: the galactic bulge transient monitor mission." In SPIE Astronomical Telescopes + Instrumentation, edited by Guenther Hasinger and Martin J. L. Turner. SPIE, 2004. http://dx.doi.org/10.1117/12.549890.

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Sellwood, J. A. "A bar model for the Galactic bulge." In Back to the Galaxy. AIP, 1992. http://dx.doi.org/10.1063/1.44022.

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Peletier, Reynier, Marc Balcells, Jesus Falcon-Barroso, and Alister Graham. "The formation of galactic bulges." In Baryons in Dark Matter Halos. Trieste, Italy: Sissa Medialab, 2004. http://dx.doi.org/10.22323/1.014.0060.

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Barragan, Laura, Erik Kuulkers, Peter Kretschmar, Joern Wilms, Katja Pottschmidt, and Anne M. Lohfink. "The INTEGRAL Galactic Bulge monitoring program: Spectral study." In 8th INTEGRAL Workshop “The Restless Gamma-ray Universe”. Trieste, Italy: Sissa Medialab, 2011. http://dx.doi.org/10.22323/1.115.0144.

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Johnson, Jeniffer. "Abundances in Galactic Bulge Dwarfs and the Origin of the Elements in the Bulge." In 10th Symposium on Nuclei in the Cosmos. Trieste, Italy: Sissa Medialab, 2009. http://dx.doi.org/10.22323/1.053.0024.

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Calchi Novati, Sebastiano. "Microlensing towards the Galactic centre an analysis of the Galactic Bulge IMF." In The Manchester Microlensing Conference: The 12th International Conference and ANGLES Microlensing Workshop. Trieste, Italy: Sissa Medialab, 2008. http://dx.doi.org/10.22323/1.054.0021.

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Reports on the topic "Galactis bulge"

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Street, R., E. T. Al, N. R. Golovich, and W. A. Dawson. Unique Science from a Coordinated LSST-WFIRST Survey of the Galactic Bulge. Office of Scientific and Technical Information (OSTI), October 2019. http://dx.doi.org/10.2172/1572250.

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Popowski, P. Microlensing Optical Depth Towards the Galactic Bulge Using Clump Giants from the MACHO Survey. Office of Scientific and Technical Information (OSTI), October 2004. http://dx.doi.org/10.2172/839963.

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