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Journal articles on the topic 'Pre-main-sequence'

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Published: 4 June 2021

Last updated: 14 March 2023

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1

Duchêne, Gaspard. "Pre-main sequence disks." Proceedings of the International Astronomical Union 6, S270 (May 2010): 45–48. http://dx.doi.org/10.1017/s1743921311000159.

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AbstractIn this contribution, I briefly review our empirical knowledge of disks around ≲2M⊙ pre-main sequence (T Tauri) stars, focusing first on the dichotomic question of their frequency before moving on to some more detailed disk properties (overall orientation, total mass, outer radius). Finally, I conclude with a brief discussion of disks around embedded protostars, which will play in the next few years a major role in testing star formation theory and simulations.

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2

Masson, Colin R. "Pre-main-sequence outflows." Astrophysics and Space Science 224, no. 1-2 (February 1995): 99–108. http://dx.doi.org/10.1007/bf00667830.

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3

D’Antona, Francesca. "The Pre - Main Sequence." International Astronomical Union Colloquium 137 (1993): 395–409. http://dx.doi.org/10.1017/s0252921100018157.

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AbstractThe Pre-Main-Sequence (pre-MS) is defined as the phase following the protostellar stage and ending with the ignition of hydrogen in the stellar core. Models in hydrostatic and thermal equilibrium such as typical “Hayashi track” models are basically adequate to describe the internal structure of pre-MS stars, although for a fraction of pre-MS objects there can be phases of accretion also at late stages, which may influence the surface abundances of light elements.The interior evolution of pre-MS structures is focused in the two main stages’ of Deuterium and Lithium burning for the low mass (M ≤ 1.5M⊙) stars. The location in the HR diagram of theoretical tracks is still subject to large uncertainty, even more apparent today that new opacities and treatment of turbulent convection are available, and the results can be internally compared. Uncertainties amount to a factor ~ two for mass and age determination of individual objects, and affect the absolute location for both the D-burning and the Li-burning regions. Qualitative constraints, such as that there can not be Li-depletion at L ≥ L⊙, remain valid. Abundances of7Li at the surface of pre-MS stars, if measured at a stage which can definitely be considered previous to the possible occurrence of nuclear burning, and, consequently, previous to other depletion mechanism which may occur later on, provide constraints on galactic evolution of this element of cosmological interest.

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4

Scicluna, P., G. Rosotti, J. E. Dale, and L. Testi. "Old pre-main-sequence stars." Astronomy & Astrophysics 566 (June 2014): L3. http://dx.doi.org/10.1051/0004-6361/201423654.

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5

Mathieu, Robert D. "Pre-Main-Sequence Binary Stars." Annual Review of Astronomy and Astrophysics 32, no. 1 (September 1994): 465–530. http://dx.doi.org/10.1146/annurev.aa.32.090194.002341.

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6

Bouy, Hervé. "Pre-main sequence multiple systems." Proceedings of the International Astronomical Union 6, S270 (May 2010): 41–44. http://dx.doi.org/10.1017/s1743921311000147.

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AbstractIt is now well established that the majority of young stars are found in multiple systems, so that any theory of stellar formation must account for their existence and properties. Studying the properties of multiple star systems therefore represents a very powerful approach to place observational constraints on star formation theories. Additionally, multiple systems offer other advantages. They provide the most accurate and unambiguous way to measure masses, using orbital fitting and Kepler's laws, and even the stellar radius in the special case of eclipsing binaries. They also allow to compare the properties of 2 coeval objects with different masses, providing important tests for the evolutionary models.

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7

Zwintz, K. "Asteroseismology of pre-main sequence stars." Communications in Asteroseismology 159 (2009): 59–60. http://dx.doi.org/10.1553/cia159s59.

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8

Hartmann, Lee, Gregory Herczeg, and Nuria Calvet. "Accretion onto Pre-Main-Sequence Stars." Annual Review of Astronomy and Astrophysics 54, no. 1 (September 19, 2016): 135–80. http://dx.doi.org/10.1146/annurev-astro-081915-023347.

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9

Marconi, Marcella, and Francesco Palla. "Pre-Main-Sequence A-type stars." Proceedings of the International Astronomical Union 2004, IAUS224 (July 2004): 69–79. http://dx.doi.org/10.1017/s1743921304004399.

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10

Zwintz, Konstanze. "Pulsation in pre-main sequence stars." Proceedings of the International Astronomical Union 11, A29B (August 2015): 552–59. http://dx.doi.org/10.1017/s1743921316006116.

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AbstractAsteroseismology has been proven to be a successful tool to unravel details of the internal structure for different types of stars in various stages of evolution well after birth. We can now show that it has similar power for pre-main sequence (pre-MS) objects. Pre-MS stars with masses between ~1 and 6 solar masses that have recently been formed and gain their energy mainly from gravitational contraction can become vibrationally unstable during their evolution to the main sequence. Within the past ~15 years, several dozens of pulsating pre-MS stars were discovered using data obtained from ground and from space. Depending on their masses, pre-MS stars can show three different types of pulsations: (i) δ Scuti type p-mode pulsations, (ii) γ Doradus like g-mode oscillations and (iii) g-mode Slowly Pulsating B star pulsations.Our asteroseismic investigations yielded new insights into the connection between the pulsations and early stellar evolution: We revealed a relation between the stars' oscillatory behavior and their relative evolutionary stages that might lead us to a model-independent determination of the stars' fundamental parameters. With this we will be able to put constraints on theoretical models and help to answer some of the yet open questions in early stellar evolution.

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11

Kenyon, Scott. "Disks in pre-main sequence stars." Astrophysics and Space Science 223, no. 1-2 (January 1995): 3–13. http://dx.doi.org/10.1007/bf00989148.

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12

Carter, B. D., and B. J. O'Mara. "An emission sequence in pre-main-sequence flare stars." Monthly Notices of the Royal Astronomical Society 253, no. 1 (November 1991): 47–54. http://dx.doi.org/10.1093/mnras/253.1.47.

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13

Grigahcéne, A. "Instability strip for pre-main-sequence stars." Communications in Asteroseismology 147 (2007): 69–71. http://dx.doi.org/10.1553/cia147s69.

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14

Vick, M., G. Michaud, J. Richer, and O. Richard. "Abundance anomalies in pre-main-sequence stars." Astronomy & Astrophysics 526 (December 17, 2010): A37. http://dx.doi.org/10.1051/0004-6361/201015533.

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15

Herbig, G. H., and S. E. Dahm. "The Pre-Main-Sequence Population of L988." Astronomical Journal 131, no. 3 (March 2006): 1530–43. http://dx.doi.org/10.1086/499809.

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16

Adams, Fred C., Michael J. Cai, Daniele Galli, Susana Lizano, and Frank H. Shu. "MAGNETIC INTERACTIONS IN PRE-MAIN-SEQUENCE BINARIES." Astrophysical Journal 743, no. 2 (December 2, 2011): 175. http://dx.doi.org/10.1088/0004-637x/743/2/175.

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17

Tayler, R. J. "Magnetic activity in pre-main-sequence stars." Monthly Notices of the Royal Astronomical Society 227, no. 3 (August 1, 1987): 553–61. http://dx.doi.org/10.1093/mnras/227.3.553.

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18

Schaefer, G. H., L. Prato, M. Simon, and J. Patience. "ORBITAL MOTION IN PRE-MAIN SEQUENCE BINARIES." Astronomical Journal 147, no. 6 (May 13, 2014): 157. http://dx.doi.org/10.1088/0004-6256/147/6/157.

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19

Hartigan, Patrick, Karen M. Strom, and Stephen E. Strom. "Are wide pre-main-sequence binaries coeval?" Astrophysical Journal 427 (June 1994): 961. http://dx.doi.org/10.1086/174203.

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20

Wichmann, R., U. Bastian, J. Krautter, I. Jankovics, and S. M. Rucinski. "Hipparcos observations of pre-main-sequence stars." Monthly Notices of the Royal Astronomical Society 301, no. 2 (December 1998): L39—L43. http://dx.doi.org/10.1046/j.1365-8711.1998.02162.x.

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21

Ducourant, C., R. Teixeira, J. P. Périé, J. F. Lecampion, J. Guibert, and M. J. Sartori. "Pre-main sequence star Proper Motion Catalogue." Astronomy & Astrophysics 438, no. 2 (July 8, 2005): 769–78. http://dx.doi.org/10.1051/0004-6361:20052788.

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22

Tout, Christopher A., Mario Livio, and Ian A. Bonnell. "The ages of pre-main-sequence stars." Monthly Notices of the Royal Astronomical Society 310, no. 2 (December 1, 1999): 360–76. http://dx.doi.org/10.1046/j.1365-8711.1999.02987.x.

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23

Palla, F. "The Physics of Pre-Main-Sequence Evolution." EAS Publications Series 3 (2002): 111–45. http://dx.doi.org/10.1051/eas:2002048.

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24

Ramírez-Tannus, M. C., L. Kaper, A. de Koter, F. Tramper, H. Sana, O. H. Ramírez-Agudelo, A. Bik, L. E. Ellerbroek, and B. B. Ochsendorf. "Massive pre-main-sequence stars in M17." Proceedings of the International Astronomical Union 12, S329 (November 2016): 439. http://dx.doi.org/10.1017/s1743921317002897.

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We obtained VLT/X-shooter spectra of twelve candidate young massive stars previously selected by Hanson et al. (1997) in the giant Hii region M17. An analysis of their spectra using FASTWIND models (Puls et al. 2005) shows that they span a mass range of 6 - 20 M⊙. We identify the presence of gaseous and dusty disks around six sources based on emission lines in the spectrum and infrared continuum excess.

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25

D. Feigelson, Eric. "Magnetic Activity of Pre-main Sequence Stars." Symposium - International Astronomical Union 219 (2004): 211–22. http://dx.doi.org/10.1017/s0074180900182130.

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I review here recent advances in our understanding of magnetic activity in pre-main sequence (PMS) protostars and T Tauri stars. Results are based on recent imaging, spectroscopic and temporal studies of nearby star forming regions from the Chandra X — ray Observatory and XMM — Newton, including a first look at an ultradeep Chandra exposure of the Orion Nebula Cluster.Pre-main sequence stars exhibit a high level of X-ray emission dominated by a bewildering variety of magnetic reconnection flares. Activity is linked to bulk stellar properties — Lbol, mass, surface area or volume — rather than rotation. This suggests that dynamo processes in deeply convective PMS stars may fundamentally differ from the tachocline dynamo operating in main sequence stars.X-rays and MeV particles from magnetic flares will affect the circumstellar environment in PMS systems, particularly the protoplanetary disk. X-ray emission may influence: disk ionization, turbulence and viscosity; Jovian planet formation and migration; the production of meteoritic isotopes and melting of meteoritic chondrules; the heating and chemistry of the disk. X-ray surveys are also effective in locating post-T Tauri stars for disk evolution studies.

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26

Miroshnichenko, A. S., K. S. Bjorkman, E. L. Chentsov, V. G. Klochkova, R. O. Gray, P. García-Lario, and J. V. Perea Calderón. "The pre-main-sequence star IP Persei." Astronomy & Astrophysics 377, no. 3 (October 2001): 854–67. http://dx.doi.org/10.1051/0004-6361:20010958.

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27

Melo, C. H. F., E. Covino, J. M. Alcalá, and G. Torres. "On the pre-main sequence circularization period." Astronomy & Astrophysics 378, no. 3 (November 2001): 898–906. http://dx.doi.org/10.1051/0004-6361:20011262.

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28

Graham, J. A. "Clumpy accretion onto pre-main-sequence stars." Publications of the Astronomical Society of the Pacific 104 (July 1992): 479. http://dx.doi.org/10.1086/133021.

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29

Lorenzetti, Dario. "Pre-Main Sequence Stars Seen by ISO." Space Science Reviews 119, no. 1-4 (August 2005): 181–99. http://dx.doi.org/10.1007/s11214-005-8064-z.

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30

Wolf, Sebastian, Bringfried Stecklum, and Thomas Henning. "Pre-Main Sequence Binaries with Aligned Disks?" Symposium - International Astronomical Union 200 (2001): 295–304. http://dx.doi.org/10.1017/s0074180900225345.

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We present the results of a study performed with the goal to investigate whether low-mass pre-main sequence binary stars are formed by multiple fragmentation or via stellar capture. If binaries form preferentially by fragmentation, we expect their disks to be co-planar. On the other hand, the capture scenario will lead to a random distribution of disk orientations. We performed near-infrared polarization measurements of 49 young visual binary stars in the K band with SOFI at the NTT. The near-infrared excess radiation of the targets mostly point to the presence of disks. For a major fraction of the sample, evidence for disks is also obvious from other features (outflows, jets, Herbig-Haro objects). We derived the disk orientation from the orientation of the polarization vector of both components of each binary. This statistical study allows to test which hypothesis (co-planarity, random orientation) is consistent with the observed distribution of polarimetric position angles. We find evidence that the disks are preferentially aligned.

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31

Zinnecker, H., A. Chelli, L. Carrasco, I. Cruz-Gonzalez, and C. Perrier. "Infrared companions to pre-main sequence stars." Astrophysics and Space Science 142, no. 1-2 (March 1988): 231. http://dx.doi.org/10.1007/bf00656214.

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32

Stahler, Steven W. "Luminosity jumps in pre-main-sequence stars." Astrophysical Journal 347 (December 1989): 950. http://dx.doi.org/10.1086/168186.

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33

Ramírez-Tannus, M. C., L. Kaper, A. de Koter, F. Tramper, A. Bik, L. E. Ellerbroek, B. B. Ochsendorf, O. H. Ramírez-Agudelo, and H. Sana. "Massive pre-main-sequence stars in M17." Astronomy & Astrophysics 604 (August 2017): A78. http://dx.doi.org/10.1051/0004-6361/201629503.

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34

Delgado, A. J., E. J. Alfaro, and J. L. Yun. "Pre-main sequence stars in open clusters." Astronomy & Astrophysics 467, no. 3 (March 13, 2007): 1397–407. http://dx.doi.org/10.1051/0004-6361:20066640.

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35

Bhattacharyya, Suman, Blesson Mathew, Gourav Banerjee, R. Anusha, K. T. Paul, and Sreeja S. Kartha. "Identification of emission-line stars in transition phase from pre-main sequence to main sequence." Monthly Notices of the Royal Astronomical Society 507, no. 3 (August 23, 2021): 3660–71. http://dx.doi.org/10.1093/mnras/stab2385.

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ABSTRACT Pre-main-sequence (PMS) stars evolve into main-sequence (MS) phase over a period of time. Interestingly, we found a scarcity of studies in existing literature that examine and attempt to better understand the stars in PMS to MS transition phase. The purpose of this study is to detect such rare stars, which we named as ‘transition phase’ (TP) candidates – stars evolving from the PMS to the MS phase. We identified 98 TP candidates using photometric analysis of a sample of 2167 classical Be (CBe) and 225 Herbig Ae/Be (HAeBe) stars. This identification is done by analysing the near- and mid-infrared excess and their location in the optical colour–magnitude diagram. The age and mass of 58 of these TP candidates are determined to be between 0.1–5 Myr and 2–10.5 M⊙, respectively. The TP candidates are found to possess rotational velocity and colour excess values in between CBe and HAeBe stars, which is reconfirmed by generating a set of synthetic samples using the machine learning approach.

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36

Alves, Joao, Lee Hartmann, Cesar Briceno, and Charles J. Lada. "Optical Outburst of a Pre-Main-Sequence Object." Astronomical Journal 113 (April 1997): 1395. http://dx.doi.org/10.1086/118354.

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37

Monin, J. L., F. Ménard, and N. Peretto. "Disc orientations in pre-main-sequence multiple systems." Astronomy & Astrophysics 446, no. 1 (January 2006): 201–10. http://dx.doi.org/10.1051/0004-6361:20042584.

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38

Tognelli, E., P. G. Prada Moroni, and S. Degl’Innocenti. "The Pisa pre-main sequence tracks and isochrones." Astronomy & Astrophysics 533 (September 2011): A109. http://dx.doi.org/10.1051/0004-6361/200913913.

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39

Castelaz, M. W., G. L. Grasdalen, J. A. Hackwell, R. W. Capps, and D. Thompson. "GL 961-W - A pre-main-sequence object." Astronomical Journal 90 (June 1985): 1113. http://dx.doi.org/10.1086/113818.

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40

Hartmann, Lee, S. T. Megeath, Lori Allen, Kevin Luhman, Nuria Calvet, Paola D’Alessio, Ramiro Franco‐Hernandez, and Giovanni Fazio. "IRAC Observations of Taurus Pre–Main‐Sequence Stars." Astrophysical Journal 629, no. 2 (August 20, 2005): 881–96. http://dx.doi.org/10.1086/431472.

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41

Zwintz, Konstanze, D. B. Guenther, and W. W. Weiss. "Nonradial Oscillations on a Pre–Main‐Sequence Star." Astrophysical Journal 655, no. 1 (January 20, 2007): 342–44. http://dx.doi.org/10.1086/509819.

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42

Ramirez, Ramses M., and Lisa Kaltenegger. "THE HABITABLE ZONES OF PRE-MAIN-SEQUENCE STARS." Astrophysical Journal 797, no. 2 (December 9, 2014): L25. http://dx.doi.org/10.1088/2041-8205/797/2/l25.

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43

Kunitomo, Masanobu, Tristan Guillot, Shigeru Ida, and Taku Takeuchi. "Revisiting the pre-main-sequence evolution of stars." Astronomy & Astrophysics 618 (October 2018): A132. http://dx.doi.org/10.1051/0004-6361/201833127.

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Aims. We want to investigate how planet formation is imprinted on stellar surface composition using up-to-date stellar evolution models. Methods. We simulate the evolution of pre-main-sequence stars as a function of the efficiency of heat injection during accretion, the deuterium mass fraction, and the stellar mass, M⋆. For simplicity, we assume that planet formation leads to the late accretion of zero-metallicity gas, diluting the surface stellar composition as a function of the mass of the stellar outer convective zone. We estimate that in the solar system, between 97 and 168 M⊕ of condensates formed planets or were ejected from the system. We adopt 150 M⊕(M⋆/M⊙)(Z/Z⊙) as an uncertain but plausible estimate of the mass of heavy elements that is not accreted by stars with giant planets, including our Sun. By combining our stellar evolution models to these estimates, we evaluate the consequences of planet formation on stellar surface composition. Results. We show that after the first ~0.1 Myr during which stellar structure can differ widely from the usually assumed fully convective structure, the evolution of the convective zone follows classical pre-main-sequence evolutionary tracks within a factor of two in age. We find that planet formation should lead to a scatter in stellar surface composition that is larger for high-mass stars than for low-mass stars. We predict a spread in [Fe/H] of approximately 0.05 dex for stars with a temperature of Teff ~ 6500 K, to 0.02 dex for stars with Teff ~ 5500 K, marginally compatible with differences in metallicities observed in some binary stars with planets. Stars with Teff ≤ 7000 K may show much larger [Fe/H] deficits, by 0.6 dex or more, in the presence of efficient planet formation, compatible with the existence of refractory-poor λ Boo stars. We also find that planet formation may explain the lack of refractory elements seen in the Sun as compared to solar twins, but only if the ice-to-rock ratio in the solar-system planets is less than ≈0.4 and planet formation began less than ≈1.3 Myr after the beginning of the formation of the Sun.

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44

Bonnell, I. A., K. W. Smith, M. R. Meyer, C. A. Tout, D. F. M. Folha, and J. P. Emerson. "Magnetospheric accretion and pre-main-sequence stellar masses." Monthly Notices of the Royal Astronomical Society 299, no. 4 (October 1, 1998): 1013–18. http://dx.doi.org/10.1046/j.1365-8711.1998.01855.x.

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45

Hartmann, L., and J. R. Stauffer. "Additional measurements of pre-main-sequence stellar rotation." Astronomical Journal 97 (March 1989): 873. http://dx.doi.org/10.1086/115033.

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46

Eggen, Olin J. "Pre-Main-Sequence Stars in the Pleiades Supercluster." Astronomical Journal 110 (October 1995): 1749. http://dx.doi.org/10.1086/117647.

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47

Popham, Robert, Ramesh Narayan, Lee Hartmann, and Scott Kenyon. "Boundary Layers in Pre-Main-Sequence Accretion Disks." Astrophysical Journal 415 (October 1993): L127. http://dx.doi.org/10.1086/187049.

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48

Ardila, David R., Christopher Jonhs-Krull, Gregory J. Herczeg, Robert D. Mathieu, and Alberto Quijano-Vodniza. "MAGNETOSPHERIC ACCRETION IN CLOSE PRE-MAIN-SEQUENCE BINARIES." Astrophysical Journal 811, no. 2 (September 29, 2015): 131. http://dx.doi.org/10.1088/0004-637x/811/2/131.

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49

Tognelli, E., S. Degl’Innocenti, and P. G. Prada Moroni. "7Li surface abundance in pre-main sequence stars." Astronomy & Astrophysics 548 (November 16, 2012): A41. http://dx.doi.org/10.1051/0004-6361/201219111.

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50

Flaccomio, E., G. Micela, and S. Sciortino. "X-ray variability of pre-main-sequence stars." Astronomy & Astrophysics 548 (November 27, 2012): A85. http://dx.doi.org/10.1051/0004-6361/201219362.

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