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Journal articles on the topic 'Star fields'

Author: Grafiati
Published: 4 June 2021
Last updated: 1 February 2022

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1

Clem, James L., and Arlo U. Landolt. "FAINTUBVRISTANDARD STAR FIELDS." Astronomical Journal 146, no. 4 (September 5, 2013): 88. http://dx.doi.org/10.1088/0004-6256/146/4/88.

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2

Hubrig, Swetlana, Markus Schöller, and Silva P. Järvinen. "Magnetic massive stars in star forming regions." Proceedings of the International Astronomical Union 14, A30 (August 2018): 132. http://dx.doi.org/10.1017/s174392131900382x.

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AbstractOne idea for the origin of magnetic fields in massive stars suggests that the magnetic field is the fossil remnant of the Galactic ISM magnetic field, amplified during the collapse of the magnetised gas cloud. A search for the presence of magnetic fields in massive stars located in active sites of star formation led to the detection of rather strong magnetic fields in a few young stars. Future spectropolarimetric observations are urgently needed to obtain insights into the mechanisms that drive the generation of kG magnetic fields during high-mass star formation.
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3

Gourgouliatos, Konstantinos N., Rainer Hollerbach, and Robert F. Archibald. "Modelling neutron star magnetic fields." Astronomy & Geophysics 59, no. 5 (October 1, 2018): 5.37–5.42. http://dx.doi.org/10.1093/astrogeo/aty235.

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4

Van Loo, S., T. W. Hartquist, and S. A. E. G. Falle. "Magnetic fields and star formation." Astronomy & Geophysics 53, no. 5 (September 18, 2012): 5.31–5.36. http://dx.doi.org/10.1111/j.1468-4004.2012.53531.x.

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5

Bellazzini, B., and M. Mintchev. "Quantum fields on star graphs." Journal of Physics A: Mathematical and General 39, no. 35 (August 11, 2006): 11101–17. http://dx.doi.org/10.1088/0305-4470/39/35/011.

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6

Zhang, Qizhou. "Magnetic fields and massive star formation." Proceedings of the International Astronomical Union 14, A30 (August 2018): 141. http://dx.doi.org/10.1017/s1743921319003922.

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AbstractMassive stars ( ${\rm{M}} > \,8{M_ \odot }$ ) often form in parsec-scale molecular clumps that collapse and fragment, leading to the birth of a cluster of stellar objects. The role of magnetic fields during the formation of massive dense cores is still not clear. The steady improvement in sensitivity of (sub)millimeter interferometers over the past decade enabled observations of dust polarization of large samples of massive star formation regions. We carried out a polarimetric survey with the Submillimeter Array of 14 massive star forming clumps in continuum emission at a wavelength of 0.89 mm. This unprecedentedly large sample of massive star forming regions observed by a submillimeter interferometer before the advent of ALMA revealed compelling evidence of strong magnetic influence on the gas dynamics from 1 pc to 0.1 pc scales. We found that the magnetic fields in dense cores tend to be either parallel or perpendicular to the mean magnetic fields in their parental molecular clumps. Furthermore, the main axis of protostellar outflows does not appear to be aligned with the mean magnetic fields in the dense core where outflows are launched. These findings suggest that from 1 pc to 0.1 pc scales, magnetic fields are dynamically important in the collapse of clumps and the formation of dense cores. From the dense core scale to the accretion disk scale of ∼102 au, however, gravity and angular momentum appear to be more dominant relative to the magnetic field.
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7

Crutcher, Richard M. "Magnetic fields and massive star formation." Proceedings of the International Astronomical Union 1, S227 (May 2005): 98–107. http://dx.doi.org/10.1017/s1743921305004412.

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8

Feitzinger, J. V., E. Harfst, and J. Spicker. "Stochastic Star Formation and Magnetic Fields." Symposium - International Astronomical Union 140 (1990): 257–58. http://dx.doi.org/10.1017/s0074180900190175.

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The model of selfpropagating star formation uses local processes (200 pc cell size) in the interstellar medium to simulate the large scale cooperative behaviour of spiral structure in galaxies. The dynamic of the model galaxies is taken into account via the mass distribution and the resulting rotation curve; flat rotation curves are used. The interstellar medium is treated as a multiphase medium with appropriate cooling times and density history. The phases are: molecular gas, cool HI gas, warm intercloud and HII gas and hot coronal fountain gas. A detailed gas reshuffeling between the star forming cells in the plane and outside the galactic plane controls the cell content. Two processes working stochastically are incooperated: the building and the decay of molecular clouds and the star forming events in the molecular clouds.
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9

Yakovlev, D. G., and A. D. Kaminker. "Neutron Star Crusts With Magnetic Fields." International Astronomical Union Colloquium 147 (1994): 214–38. http://dx.doi.org/10.1017/s0252921100026385.

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AbstractThe properties of plasma in neutron star crusts with strong magnetic fields B = 1010 − 1013 G are reviewed: thermodynamic properties (equation of state, entropy, specific heat), transport properties (electron thermal and electrical conductivity of degenerate electron gas, radiative thermal conductivity of very surface nondegenerate layers) and neutrino energy losses. Classical effects of electron Larmor rotation in a magnetic field are considered as well as quantum effects of the electron motion (Landau levels). The influence of the magnetic fields on density and temperature profiles in the surface layers of neutron stars and on neutron star cooling is briefly discussed.
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10

Michel, F. C. "Evolution of Neutron Star Magnetic Fields." Publications of the Astronomical Society of the Pacific 103 (August 1991): 770. http://dx.doi.org/10.1086/132877.

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11

Johns–Krull, Christopher M. "Measuring T Tauri star magnetic fields." Proceedings of the International Astronomical Union 4, S259 (November 2008): 345–56. http://dx.doi.org/10.1017/s1743921309030713.

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AbstractStellar magnetic fields including a strong dipole component are believed to play a critical role in the early evolution of newly formed stars and their circumstellar accretion disks. It is currently believed that the stellar magnetic field truncates the accretion disk several stellar radii above the star. This action forces accreting material to flow along the field lines and accrete onto the star preferentially at high stellar latitudes. It is also thought that the stellar rotation rate becomes locked to the Keplerian velocity near the radius where the disk is truncated. This paper reviews recent efforts to measure the magnetic field properties of low mass pre-main sequence stars, focussing on how the observations compare with the theoretical expectations. A picture is emerging indicating that quite strong fields do indeed cover the majority of the surface on these stars; however, the dipole component of the field appears to be alarmingly small. The current measurements also suggest that given their strong magnetic fields, T Tauri stars are somewhat faint in X-rays relative to what is expected from simple main sequence star scaling laws.
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12

Zhang, Qizhou, Keping Qiu, Josep M. Girart, Hauyu (Baobab) Liu, Ya-Wen Tang, Patrick M. Koch, Zhi-Yun Li, et al. "MAGNETIC FIELDS AND MASSIVE STAR FORMATION." Astrophysical Journal 792, no. 2 (August 22, 2014): 116. http://dx.doi.org/10.1088/0004-637x/792/2/116.

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13

Elmegreen, Bruce G., and Debra Meloy Elmegreen. "Fractal Structure in Galactic Star Fields." Astronomical Journal 121, no. 3 (March 2001): 1507–11. http://dx.doi.org/10.1086/319416.

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14

Baker, Andrew J., Richard I. Davies, M. D. Lehnert, N. A. Thatte, W. D. Vacca, O. R. Hainaut, M. J. Jarvis, G. K. Miley, and H. J. A. Röttgering. "Galaxies in southern bright star fields." Astronomy & Astrophysics 406, no. 2 (August 2003): 593–601. http://dx.doi.org/10.1051/0004-6361:20030812.

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15

Clem, James L., and Arlo U. Landolt. "FAINTUBVRISTANDARD STAR FIELDS AT +50° DECLINATION." Astronomical Journal 152, no. 4 (September 29, 2016): 91. http://dx.doi.org/10.3847/0004-6256/152/4/91.

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16

Usov, V. V. "Evolution of neutron star magnetic fields." Astrophysics and Space Science 140, no. 1 (1988): 39–47. http://dx.doi.org/10.1007/bf00643526.

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17

Bhattacharya, Dipankar. "Evolution of neutron star magnetic fields." Journal of Astrophysics and Astronomy 23, no. 1-2 (March 2002): 67–72. http://dx.doi.org/10.1007/bf02702467.

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18

Igoshev, Andrei P., Sergei B. Popov, and Rainer Hollerbach. "Evolution of Neutron Star Magnetic Fields." Universe 7, no. 9 (September 20, 2021): 351. http://dx.doi.org/10.3390/universe7090351.

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Neutron stars are natural physical laboratories allowing us to study a plethora of phenomena in extreme conditions. In particular, these compact objects can have very strong magnetic fields with non-trivial origin and evolution. In many respects, its magnetic field determines the appearance of a neutron star. Thus, understanding the field properties is important for the interpretation of observational data. Complementing this, observations of diverse kinds of neutron stars enable us to probe parameters of electro-dynamical processes at scales unavailable in terrestrial laboratories. In this review, we first briefly describe theoretical models of the formation and evolution of the magnetic field of neutron stars, paying special attention to field decay processes. Then, we present important observational results related to the field properties of different types of compact objects: magnetars, cooling neutron stars, radio pulsars, and sources in binary systems. After that, we discuss which observations can shed light on the obscure characteristics of neutron star magnetic fields and their behaviour. We end the review with a subjective list of open problems.
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19

Johnstone, C. P., M. Jardine, S. G. Gregory, J. F. Donati, and G. Hussain. "Classical T Tauri stars: magnetic fields, coronae and star–disc interactions." Monthly Notices of the Royal Astronomical Society 437, no. 4 (December 5, 2013): 3202–20. http://dx.doi.org/10.1093/mnras/stt2107.

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20

Käpylä, P. J. "Star-in-a-box simulations of fully convective stars." Astronomy & Astrophysics 651 (July 2021): A66. http://dx.doi.org/10.1051/0004-6361/202040049.

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Context. Main-sequence late-type stars with masses of less than 0.35 M⊙ are fully convective. Aims. The goal is to study convection, differential rotation, and dynamos as functions of rotation in fully convective stars. Methods. Three-dimensional hydrodynamic and magnetohydrodynamic numerical simulations with a star-in-a-box model, in which a spherical star is immersed inside of a Cartesian cube, are used. The model corresponds to a 0.2 M⊙ main-sequence M5 dwarf. A range of rotation periods (Prot) between 4.3 and 430 d is explored. Results. The slowly rotating model with Prot = 430 days produces anti-solar differential rotation with a slow equator and fast poles, along with predominantly axisymmetric quasi-steady large-scale magnetic fields. For intermediate rotation (Prot = 144 and 43 days) the differential rotation is solar-like (fast equator, slow poles), and the large-scale magnetic fields are mostly axisymmetric and either quasi-stationary or cyclic. The latter occurs in a similar parameter regime as in other numerical studies in spherical shells, and the cycle period is similar to observed cycles in fully convective stars with rotation periods of roughly 100 days. In the rapid rotation regime the differential rotation is weak and the large-scale magnetic fields are increasingly non-axisymmetric with a dominating m = 1 mode. This large-scale non-axisymmetric field also exhibits azimuthal dynamo waves. Conclusions. The results of the star-in-a-box models agree with simulations of partially convective late-type stars in spherical shells in that the transitions in differential rotation and dynamo regimes occur at similar rotational regimes in terms of the Coriolis (inverse Rossby) number. This similarity between partially and fully convective stars suggests that the processes generating differential rotation and large-scale magnetism are insensitive to the geometry of the star.
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21

Crutcher, Richard M. "Role of Magnetic Fields in Star Formation." Proceedings of the International Astronomical Union 5, H15 (November 2009): 438–39. http://dx.doi.org/10.1017/s1743921310010173.

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AbstractI describe two recent projects to test star formation theory using Zeeman observations. First, using Bayesian analysis, the probability distribution function of the magnitude of the total magnetic field strength Bt and its dependence on volume density n(H) were inferred from Zeeman observations of the line-of-sight strengths Bz. The result was that from one molecular cloud to another Bt ranges uniformly between values close to zero and a maximum B0, and that B0 scales as n2/3. Second, observations of the ratio of the mass/flux (M/Φ) between the core and envelope regions of four dark clouds yielded values < 1. All of these results disagree with predictions of the strong magnetic field, ambipolar diffusion driven theory of star formation.
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22

Nandi, Rana, and Debades Bandyopadhyay. "Neutron Star Crust in Strong Magnetic Fields." Journal of Physics: Conference Series 312, no. 4 (September 23, 2011): 042016. http://dx.doi.org/10.1088/1742-6596/312/4/042016.

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23

Loo, Sven Van, Jonathan C. Tan, and Sam A. E. G. Falle. "MAGNETIC FIELDS AND GALACTIC STAR FORMATION RATES." Astrophysical Journal 800, no. 1 (February 10, 2015): L11. http://dx.doi.org/10.1088/2041-8205/800/1/l11.

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24

Turk, Matthew J., Jeffrey S. Oishi, Tom Abel, and Greg L. Bryan. "MAGNETIC FIELDS IN POPULATION III STAR FORMATION." Astrophysical Journal 745, no. 2 (January 13, 2012): 154. http://dx.doi.org/10.1088/0004-637x/745/2/154.

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25

Guang-Jun, Mao, V. N. Kondratyev, A. Iwamoto, Li Zhu-Xia, Wu Xi-Zhen, W. Greiner, and I. N. Mikhailov. "Neutron Star Composition in Strong Magnetic Fields." Chinese Physics Letters 20, no. 8 (July 30, 2003): 1238–41. http://dx.doi.org/10.1088/0256-307x/20/8/315.

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26

Meintjes, P. J., and E. Jurua. "Secondary star magnetic fields in close binaries." Monthly Notices of the Royal Astronomical Society 372, no. 3 (November 1, 2006): 1279–88. http://dx.doi.org/10.1111/j.1365-2966.2006.10933.x.

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27

Curran, R. L., and A. Chrysostomou. "Magnetic fields in massive star-forming regions." Monthly Notices of the Royal Astronomical Society 382, no. 2 (December 1, 2007): 699–716. http://dx.doi.org/10.1111/j.1365-2966.2007.12399.x.

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28

Cohen, Jim. "Observing Magnetic Fields in Star-Forming Regions." Astrophysics and Space Science 295, no. 1-2 (January 2005): 27–36. http://dx.doi.org/10.1007/s10509-005-3653-6.

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29

Hussain, G. A. J. "T Tauri star magnetic fields and magnetospheres." Astronomische Nachrichten 333, no. 1 (January 2012): 4–19. http://dx.doi.org/10.1002/asna.201111627.

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30

Kontizas, M., and E. Kontizas. "Star Formation of Star Clusters in the SMC and their Adjoining Fields." Symposium - International Astronomical Union 116 (1986): 101–2. http://dx.doi.org/10.1017/s0074180900148739.

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Photometric and recent spectroscopic studies of the SMC have shown that the differences observed in the SMC clusters and those of our Galaxy could be attibuted to differences in metallicity, star formation rate and/or the Initial Mass Function (IMF) (Humphries, 1983). The studied clusters NGC152 and KRON3 are located at the west side of the bar of the SMC and their adjoining fields represent the halo population of this galaxy.
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31

Jardine, Moira, Jean-Francois Donati, Doris Arzoumanian, and Aline de Vidotto. "Modelling stellar coronal magnetic fields." Proceedings of the International Astronomical Union 6, S273 (August 2010): 242–48. http://dx.doi.org/10.1017/s1743921311015316.

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AbstractOur understanding of the structure and dynamics of stellar coronae has changed dramatically with the availability of surface maps of both star spots and also magnetic field vectors. Magnetic field extrapolations from these surface maps reveal surprising coronal structures for stars whose masses and hence internal structures and dynamo modes may be very different from that of the Sun. Crucial factors are the fraction of open magnetic flux (which determines the spin-down rate for the star as it ages) and the location and plasma density of closed-field regions, which determine the X-ray and radio emission properties. There has been recent progress in modelling stellar coronae, in particular the relative contributions of the field detected in the bright surface regions and the field that may be hidden in the dark star spots. For the Sun, the relationship between the field in the spots and the large scale field is well studied over the solar cycle. It appears, however, that other stars can show a very different relationship.
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32

Byleveld, S. E., and H. Pongracic. "The Influence of Magnetic Fields on Star Formation." Publications of the Astronomical Society of Australia 13, no. 1 (January 1996): 71–74. http://dx.doi.org/10.1017/s1323358000020567.

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AbstractNumerical simulations suggest that colliding molecular clouds induce gravitational collapse and may be responsible for star formation. We incorporate magnetic fields in these simulations and present preliminary results of an investigation of the influence of magnetic fields on star formation via this process.
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33

Crutcher, Richard M., and Thomas H. Troland. "Magnetic fields and star formation – new observational results." Proceedings of the International Astronomical Union 2, S237 (August 2006): 141–47. http://dx.doi.org/10.1017/s1743921307001366.

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AbstractAlthough the subject of this meeting is triggered star formation in a turbulent interstellar medium, it remains unsettled what role magnetic fields play in the star formation process. This paper briefly reviews star formation model predictions for the ratio of mass to magnetic flux, describes how Zeeman observations can test these predictions, describes new results – an extensive OH Zeeman survey of dark cloud cores with the Arecibo telescope, and discusses the implications. Conclusions are that the new data support and extend the conclusions based on the older observational results – that observational data on magnetic fields in molecular clouds are consistent with the strong magnetic field model of star formation. In addition, the observational data on magnetic field strengths in the interstellar medium strongly suggest that molecular clouds must form primarily by accumulation of matter along field lines. Finally, a future observational project is described that could definitively test the ambipolar diffusion model for the formation of cores and hence of stars.
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34

Somayehee, Farshad, Amir Ali Nikkhah, and Jafar Roshanian. "Uniform Star Catalogue using GWKM Clustering for Application in Star Sensors." Journal of Navigation 72, no. 04 (January 21, 2019): 948–64. http://dx.doi.org/10.1017/s0373463318001029.

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In this paper, a novel algorithm of weighted k-means clustering with geodesic criteria is presented to generate a uniform database for a star sensor. For this purpose, selecting the appropriate star catalogue and desirable minimum magnitude and eliminating double stars are among the steps of the uniformity process. Further, Delaunay triangulation and determining the scattered data density by using a Voronoi diagram were used to solve the problems of the proposed clustering method. Thus, by running a Monte Carlo simulation to count the number of stars observed in different fields of view, it was found that the uniformity leads to a significant reduction of the probability of observing a large number of stars in all fields of view. In contrast, the uniformity slightly increased the field of view needed to observe the minimum number of required stars for an identification algorithm.
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35

Pudritz, Ralph E., Mikhail Klassen, Helen Kirk, Daniel Seifried, and Robi Banerjee. "The Role of Magnetic Fields in Star Formation." Proceedings of the International Astronomical Union 9, S302 (August 2013): 10–20. http://dx.doi.org/10.1017/s174392131400163x.

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AbstractStars are born in turbulent, magnetized filamentary molecular clouds, typically as members of star clusters. Several remarkable technical advances enable observations of magnetic structure and field strengths across many physical scales, from galactic scales on which giant molecular clouds (GMCs) are assembled, down to the surfaces of magnetized accreting young stars. These are shedding new light on the role of magnetic fields in star formation. Magnetic fields affect the gravitational fragmentation and formation of filamentary molecular clouds, the formation and fragmentation of magnetized disks, and finally to the shedding of excess angular momentum in jets and outflows from both the disks and young stars. Magnetic fields play a particularly important role in angular momentum transport on all of these scales. Numerical simulations have provided an important tool for tracking the complex process of the collapse and evolution of protostellar gas since several competing physical processes are at play - turbulence, gravity, MHD, and radiation fields. This paper focuses on the role of magnetic fields in three crucial regimes of star formation: the formation of star clusters emphasizing fragmentation, disk formation and the origin of early jets and outflows, to processes that control the spin evolution of young stars.
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36

Barker, Paul K. "Magnetic Fields in Be Stars? (Review Paper)." International Astronomical Union Colloquium 92 (August 1987): 38–48. http://dx.doi.org/10.1017/s0252921100115982.

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AbstractNo mean longitudinal or toroidal magnetic fields have yet been detected on any classical Be star. Models of stellar winds and circumstellar envelopes around magnetic Be stars are not appreciably constrained by present observed upper limits on field strength. A few magnetic Be stars do exist among the helium strong stars, but these objects show spectral phenomenology which is unmistakably distinct from that shown by every other object known as a Be star.
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37

Igoshev, A. P., and A. F. Kholtygin. "Statistics of magnetic fields and fluxes of massive OB stars and the origin of neutron star magnetic fields." Astronomische Nachrichten 332, no. 9-10 (December 2011): 1012–21. http://dx.doi.org/10.1002/asna.201111609.

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38

Gallart, Carme, Ingrid Meschin, Antonio Aparicio, Peter B. Stetson, and Sebastián L. Hidalgo. "Spatial variations in the star formation history of the Large Magellanic Cloud." Proceedings of the International Astronomical Union 4, S256 (July 2008): 281–86. http://dx.doi.org/10.1017/s1743921308028585.

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AbstractBased on the quantitative analysis of a set of wide-field color—magnitude diagrams reaching the old main sequence-turnoffs, we present new LMC star-formation histories, and their variation with galactocentric distance. Some coherent features are found, together with systematic variations of the star-formation history among the three fields analyzed. We find two main episodes of star formation in all three fields, from 1 to 4 and 7 to 13 Gyr ago, with relatively low star formation around ≃ 4–7 Gyr ago. The youngest age in each field gradually increases with galactocentric radius; in the innermost field, LMC 0514–6503, an additional star formation event younger than 1 Gyr is detected, with star formation declining, however, in the last ≃ 200 Myr. The population is found to be older on average toward the outer part of the galaxy, although star formation in all fields seems to have started around 13 Gyr ago.
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39

Frew, Eric W., and Dale Lawrence. "Tracking Dynamic Star Curves Using Guidance Vector Fields." Journal of Guidance, Control, and Dynamics 40, no. 6 (June 2017): 1488–95. http://dx.doi.org/10.2514/1.g002134.

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40

Soler, Juan D. "Observations of magnetic fields in star-forming clouds." Proceedings of the International Astronomical Union 14, A30 (August 2018): 101. http://dx.doi.org/10.1017/s1743921319003569.

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AbstractThis review examines observations of magnetic fields in molecular clouds, that is, at spatial scales ranging from tens to tenths of parsecs and densities up to hundreds of particles per cubic centimetre. I will briefly summarize the techniques for observing and mapping magnetic fields in molecular clouds. I will review important examples of observational results obtained using each technique and their implications for our understanding of the role of the magnetic field in molecular cloud formation and evolution. Finally, I will briefly discuss the prospects for advances in our observational capabilities with telescopes and instruments now beginning operation or under construction.
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41

Alford, Mark, Jürgen Berges, and Krishna Rajagopal. "Magnetic fields within color superconducting neutron star cores." Nuclear Physics B 571, no. 1-2 (April 2000): 269–84. http://dx.doi.org/10.1016/s0550-3213(99)00830-5.

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42

Frank, A., S. Li, and E. G. Blackman. "Triggered star formation: Rotation, magnetic fields and outflows." High Energy Density Physics 17 (December 2015): 12–17. http://dx.doi.org/10.1016/j.hedp.2015.01.002.

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43

Romani, Roger W., and Lars E. Hernquist. "Evolution of thermally generated neutron-star magnetic Fields." International Astronomical Union Colloquium 128 (1992): 46–48. http://dx.doi.org/10.1017/s0002731600154745.

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AbstractStrongly magnetized neutron stars are believed to underlie a variety of astrophysical systems, although conflicting observational and theoretical evidence has led to debate on the origin and stability of these magnetic fields. Here we describe a new model of neutron star magnetic moments, assuming that the fields are generated at birth and following their evolution to ages as large as the Hubble time. With realistic thermal evolution and conductivities, isolated neutron stars will maintain large magnetic dipole fields. As suggested elsewhere field modification under mass accretion might lead to torque decay. We identify an operative mechanism for this process; the results of this unified picture are in agreement with observations of a wide range of neutron star systems.
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44

Renaud, Florent, Mark Gieles, and Christian M. Boily. "Evolution of star clusters in arbitrary tidal fields." Monthly Notices of the Royal Astronomical Society 418, no. 2 (November 3, 2011): 759–69. http://dx.doi.org/10.1111/j.1365-2966.2011.19531.x.

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45

Sang, Yeming, and G. Chanmugam. "Ohmic decay of crustal neutron star magnetic fields." Astrophysical Journal 323 (December 1987): L61. http://dx.doi.org/10.1086/185057.

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46

Baumgardt, H., and J. Makino. "Dynamical evolution of star clusters in tidal fields." Monthly Notices of the Royal Astronomical Society 340, no. 1 (March 21, 2003): 227–46. http://dx.doi.org/10.1046/j.1365-8711.2003.06286.x.

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47

Wright, C. M., D. K. Aitken, C. H. Smith, and P. F. Roche. "Magnetic Fields and Disks in Star-forming Regions." Publications of the Astronomical Society of Australia 10, no. 3 (1993): 247–49. http://dx.doi.org/10.1017/s1323358000025777.

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AbstractThe star-formation process is an outstanding and largely unsolved problem in astrophysics. The role of magnetic fields is unclear but is widely considered to be important at all stages of protostellar evolution, from cloud collapse to ZAMS. For example, in some hydromagnetic models, the field may assist in removing angular momentum, thereby driving accretion and perhaps bipolar outflows.Spectropolarimetry between 8 and 13μm provides information on the direction of the transverse component of a magnetic field through the alignment of dust grains. We present results of 8–13μm spectropolarimetric observations of a number of bipolar molecular outflow sources, and compare the field directions observed with the axes of the outflows and putative disk-like structures observed to be associated with some of the objects. There is a strong correlation, though so far with limited statistics, between the magnetic field and disk orientations. We compare our results with magnetic field configurations predicted by current models for hydromagnetically driven winds from the disks around Young Stellar Objects (YSOs). Our results appear to argue against the Pudritz and Norman model and instead seem to support the Uchida and Shibata model.
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48

Noël, Noelia E. D., Antonio Aparicio, Carme Gallart, Sebastián L. Hidalgo, Edgardo Costa, and René A. Méndez. "The star formation history in 12 SMC fields." Proceedings of the International Astronomical Union 4, S256 (July 2008): 269–74. http://dx.doi.org/10.1017/s1743921308028561.

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AbstractWe present a quantitative analysis of the star formation history (SFH) of 12 fields in the Small Magellanic Cloud (SMC) based on unprecedented deep [(B–R),R] color—magnitude diagrams (CMDs) from Noël et al. (2007). Our fields reach down to the oldest main sequence (MS) turnoff with high photometric accuracy, which is vital for obtaining accurate SFHs. We use the IAC-pop code (Aparicio & Hidalgo 2009) to obtain the SFH, using a single CMD generated using IAC-star (Aparicio & Gallart 2004). We find that there are three main periods of enhancement of star formation: a young one peaked at ~0.2–0.5 Gyr old, only present in the eastern and in the central-most fields; one at intermediate ages, peaked at ~4–5 Gyr old in all fields; and an old one, peaked at ~10 Gyr in all the fields but the western ones, in which this old enhancement splits into two, peaked at ~8 Gyr old and at ~12 Gyr old. This “two-enhancement” zone seems to be a robust feature since it is unaffected when using different stellar evolutionary libraries, implying that stars in the SMC take a Hubble time or more to mix. This indicates that there was a global enhancement in ψ(t) at ~4–5 Gyr ago in the SMC. We also find that the age of the old population is similar at all radii and at all azimuth and we constrain the age of this oldest population to be older than ~11.5 Gyr old. The intermediate-age population, in turn, presents variations with both, radii and azimuth. Theoretical studies based on results from larger spatial areas are needed to understand the origin of the young gradient. This young component is highly affected by interactions between Milky Way/LMC/SMC. We do not find yet a region dominated by an old, Milky Way-like, halo at 4.5 kpc from the SMC center, indicating either that this old stellar halo does not exist in the SMC or that its contribution to the stellar populations, at the galactocentric distances of our outermost field, is negligible.
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Price, D. J. "Producing Ultrastrong Magnetic Fields in Neutron Star Mergers." Science 312, no. 5774 (May 5, 2006): 719–22. http://dx.doi.org/10.1126/science.1125201.

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50

Romani, Roger W. "A unified model of neutron-star magnetic fields." Nature 347, no. 6295 (October 1990): 741–43. http://dx.doi.org/10.1038/347741a0.

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