2017A&A...602A.120F


Query : 2017A&A...602A.120F

2017A&A...602A.120F - Astronomy and Astrophysics, volume 602A, 120-120 (2017/6-1)

Protostellar accretion traced with chemistry. High-resolution C18O and continuum observations towards deeply embedded protostars in Perseus.

FRIMANN S., JORGENSEN J.K., DUNHAM M.M., BOURKE T.L., KRISTENSEN L.E., OFFNER S.S.R., STEPHENS I.W., TOBIN J.J. and VOROBYOV E.I.

Abstract (from CDS):

Context. Understanding how accretion proceeds is a key question of star formation, with important implications for both the physical and chemical evolution of young stellar objects. In particular, very little is known about the accretion variability in the earliest stages of star formation.
Aims. Our aim is to characterise protostellar accretion histories towards individual sources by utilising sublimation and freeze-out chemistry of CO.
Methods. A sample of 24 embedded protostars are observed with the Submillimeter Array (SMA) in context of the large program "Mass Assembly of Stellar Systems and their Evolution with the SMA" (MASSES). The size of the C18O-emitting region, where CO has sublimated into the gas-phase, is measured towards each source and compared to the expected size of the region given the current luminosity. The SMA observations also include 1.3mm continuum data, which are used to investigate whether or not a link can be established between accretion bursts and massive circumstellar disks.
Results. Depending on the adopted sublimation temperature of the CO ice, between 20% and 50% of the sources in the sample show extended C18O emission indicating that the gas was warm enough in the past that CO sublimated and is currently in the process of refreezing; something which we attribute to a recent accretion burst. Given the fraction of sources with extended C18O emission, we estimate an average interval between bursts of 20000-50000yr, which is consistent with previous estimates. No clear link can be established between the presence of circumstellar disks and accretion bursts, however the three closest known binaries in the sample (projected separations <20AU) all show evidence of a past accretion burst, indicating that close binary interactions may also play a role in inducing accretion variability.

Abstract Copyright: © ESO, 2017

Journal keyword(s): stars: formation - stars: protostars - ISM: molecules - protoplanetary disks - circumstellar matter - circumstellar matter

Simbad objects: 30

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Number of rows : 30
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 IRAS 03222+3034 Y*O 03 25 22.32 +30 45 13.9           ~ 139 0
2 SSTc2d J032536.4+304522 Y*O 03 25 36.49 +30 45 22.2           ~ 193 1
3 [SDA2014] West4 Y*O 03 25 38.83 +30 44 06.2           ~ 250 1
4 SSTc2d J032539.1+304358 Y*? 03 25 39.12 +30 43 58.2           ~ 43 1
5 IRAS 03235+3004 Y*O 03 26 37.425 +30 15 28.39           ~ 81 0
6 2MASS J03283450+3100510 Y*O 03 28 34.501 +31 00 51.01           ~ 72 0
7 IRAS 03255+3103 Y*O 03 28 37.06800 +31 13 31.0044           ~ 83 1
8 2MASS J03284325+3117330 Y*O 03 28 43.2624763920 +31 17 33.138111588     17.78 16.45 15.07 K7.0 56 1
9 [JCC87] IRAS 2A Y*O 03 28 55.55 +31 14 36.7           ~ 439 3
10 V* V512 Per Or* 03 29 03.7578170808 +31 16 03.947525688           ~ 371 0
11 [JCC87] IRAS 4A Y*O 03 29 10.49 +31 13 30.8           ~ 684 1
12 [JJK2007] 23 Y*O 03 29 10.68 +31 18 20.6           ~ 38 1
13 ASR 32 Y*O 03 29 11.25 +31 18 31.7           ~ 47 1
14 NAME IRAS 4B1 South Y*O 03 29 12.06 +31 13 01.7           ~ 32 1
15 [JCC87] IRAS 4C Y*O 03 29 13.54 +31 13 58.2           ~ 99 1
16 SSTc2d J032923.5+313330 Y*O 03 29 23.47 +31 33 29.5           ~ 38 1
17 IRAS 03282+3035 cor 03 31 20.98 +30 45 30.1           ~ 168 0
18 IRAS 03292+3039 cor 03 32 17.96 +30 49 47.5           ~ 75 0
19 JCMTSE J033317.8+310932 cor 03 33 17.85 +31 09 31.9           ~ 100 0
20 NAME Perseus Cloud SFR 03 35.0 +31 13           ~ 1266 0
21 Cl* IC 348 LRL 54362 Y*O 03 43 50.96 +32 03 24.7           ~ 36 1
22 [RZP2014] JVLA 1 Y*O 03 43 51.02 +32 03 08.1           ~ 38 2
23 HH 211 Y*O 03 43 56.52 +32 00 52.8           ~ 343 0
24 NAME IC 348 MMS cor 03 43 56.84 +32 03 04.7           ~ 75 1
25 Cl* IC 348 LRL 1889 Y*O 03 44 21.353 +31 59 32.73           ~ 33 1
26 IRAS 03445+3242 Y*O 03 47 41.603 +32 51 43.79           ~ 192 0
27 HOPS 383 Y*O 05 35 29.8407 -04 59 51.006           ~ 58 0
28 V* FU Ori Or* 05 45 22.3647842544 +09 04 12.291320064   10.72 9.60     F0Iab 774 1
29 Lupus 1 Cld 15 43 02.1 -34 09 06           ~ 263 0
30 IRAS 15398-3359 Y*? 15 43 02.21016 -34 09 07.7112       18.38 21.72 ~ 156 0

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2023.01.31-08:37:03

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