V1647 Orionis: Reinvigorated Accretion and the Re-Appearance of McNeil's Nebula

Aspin, C.; Reipurth, Bo; Beck, Tracy; Aldering, G.; Doering, Ryan L.; Hammel, Heidi B.; Lynch, D. K.; Meixner, Margaret; Pécontal, É.; Russell, R. W.; Sitko, Michael L.; Thomas, R. C.; Vivian, U

doi:10.1088/0004-637x/692/2/l67

Cited by 42 publications

(35 citation statements)

References 29 publications

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“…In recent studies, such a scenario is used to explain the light variability of two PMS objects with characteristics similar to those of FUor and EXor -V1647 Ori (Aspin et al 2009b;Aspin 2011) and V2492 Cyg (Hillenbrand et al 2013;Kóspál et al 2013). It seems that the time variable extinction is characteristic not only of some Herbig Ae/Be stars (UXor variables) but is also a common phenomenon during the evolution of all types of PMS stars.…”

Section: Discussionmentioning

confidence: 99%

Photometric and spectroscopic variability of the FUor star V582 Aurigae

Semkov¹,

Peneva²,

Munari³

et al. 2013

A&A

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Aims. We present results from optical photometric and spectroscopic observations of the eruptive pre-main sequence star V582 Aur. Variability of the star was reported a few years ago when it was suspected as a possible FU Orionis object. Due to the small number of currently known FUors, a new object of this type is ideal target for follow-up photometric and spectroscopic observations. Methods. We carried out BVRI CCD photometric observations in the field of V582 Aur from 2009 August to 2013 February. We acquired high-, medium-, and low-resolution spectroscopy of V582 Aur during this period. To study the pre-outburst variability of the target and construct its historical light curve, we searched for archival observations in photographic plate collections. Both CCD and photographic observations were analyzed using a sequence of 14 stars in the field of V582 Aur calibrated in BVRI. Results. The pre-outburst photographic observations of V582 Aur show low-amplitude light variations typical of T Tauri stars. Archival photographic observations indicate that the increase in brightness began in late 1984 or early 1985 and the star reached the maximum level of brightness at 1986 January. The spectral type of V582 Aur can be defined as G0I with strong P Cyg profiles of Hα and Na I D lines, which are typical of FU Orionis objects. Our BVRI photometric observations show large amplitude variations (ΔV ∼ 2. m 8) during the 3.5 year period of observations. Most of the time, however, the star remains in a state close to the maximum brightness. The deepest drop in brightness was observed in the spring of 2012, when the brightness of the star fell to a level close to the pre-outburst. The multicolor photometric data show a color reversal during the minimum in brightness, which is typical of UX Ori variables. The corresponding spectral observations show strong variability in the profiles and intensities of the spectral lines (especially Hα), which indicate significant changes in the accretion rate. On the basis of photometric monitoring performed over the past three years, the spectral properties of the maximal light, and the shape of the long-term light curve, we confirm the affiliation of V582 Aur to the group of FU Orionis objects.

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Section: Discussionmentioning

confidence: 99%

Photometric and spectroscopic variability of the FUor star V582 Aurigae

Semkov¹,

Peneva²,

Munari³

et al. 2013

A&A

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“…In the NIR, V1647 Ori possessed strong emission in Brγ , Na i, and the v = 2−0 CO overtone bandheads, all indications were that the emission region was hot, extremely dense, and in an excited kinematic state. The optical brightening is attributed to a combination of the star being revealed after dust in the immediate circumstellar environment of the object was sublimated (Aspin et al 2009b) together with a luminosity increase due to the addition of significant hot accretion flux. The brightening in the NIR is perhaps more likely the effect of irradiation and subsequent heating of the inner regions of the circumstellar disk, beyond the sublimation radius, by UV flux from the accretion flow.…”

Section: Outburst Timelinementioning

confidence: 99%

“…In these research papers, considerable speculation has been put forth as to the nature of this eruptive event, yet it is generally agreed that it is the result of a rapid and massive increase in accretion onto the surface of the young star. The reader is referred to the papers byÀbrahàm et al (2004a, 2004b, 2006), Acosta-Pulido et al (2007), Andrews et al (2004), Aspin et al (2006), Aspin et al (2008, herein ABR08), Aspin et al (2009aAspin et al ( , 2009b, Briceño et al (2004), Brittain et al (2007), Fedele et al (2007aFedele et al ( , 2007b, Gibb et al (2006), Grosso et al (2005), Kastner et al (2004Kastner et al ( , 2006, Kóspál et al (2005), Kun (2008), McGehee et al (2004), Mosoni et al (2005), Muzerolle et al (2005), Ojha et al (2005Ojha et al ( , 2006, Reipurth & Aspin (2004), Rettig et al (2005), Semkov (2004Semkov ( , 2006, Tsukagoshi et al (2005), Vacca et al (2004), Vig et al (2006), and Walter et al (2004) for further discussions.…”

Section: Introduction When the Amateur Astronomer Jay Mcneil Discovermentioning

confidence: 99%

V1647 Orionis: Optical Photometric and Spectroscopic Monitoring Through the 2003-2006 Outburst

Aspin

Reipurth

2009

The Astronomical Journal

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We present results from an optical imaging and spectroscopic monitoring campaign on the young, low-mass eruptive variable star V1647 Orionis. The star and associated nebulosity (McNeil's Nebula) were observed over the period 2004 February to 2006 February with observations commencing a few months after the original outburst event occurred. Using the Gemini North telescope, we obtained multiband optical imaging photometry and medium-resolution long-slit spectroscopy of V1647 Ori on an approximately monthly interval. During this period, V1647 Ori remained at, or close to, peak brightness and then faded by 5 mag to close to its pre-outburst brightness. This implies an outburst timescale of around 27 months. Spectral features seen in both emission and absorption varied considerably during the monitoring period. For example, the Hα line changed significantly in both intensity and profile. We present and discuss the observed photometric and spectroscopic changes and consider how this eruptive event relates to the early formative stages of low-mass stars.

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“…They are thought to be active T-Tauri stars experiencing an accretion burst. Aspin et al (2009b) collected spectra of V1647 Orionis, the FUOr star responsible for the appearance of the McNeil nebula (McNeil et al 2004), and show that its CO bandheads shift from absorption to emission when the star experiences a FUOr event. Calvet et al (1991) explained theoretically this type of transition by an increase of the accretion rate.…”

Section: Spectroscopy Of Embedded Sourcesmentioning

confidence: 99%

Near-IR integral field spectroscopy of ionizing stars and young stellar objects on the borders of H II regions

Martins¹,

Pomarès²,

Deharveng³

et al. 2010

A&A

133

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Aims. We study three Galactic H ii regions -RCW 79, RCW 82, and RCW 120 -where triggered star formation is taking place. Two stellar populations are observed: the ionizing stars of each H ii region and young stellar objects on their borders. Our goal is to show that they represent two distinct populations, as expected from successive star-forming events. Methods. We use near-infrared integral field spectroscopy obtained with SINFONI on the VLT to make a spectral classification. We derived the stellar and wind properties of the ionizing stars using atmosphere models computed with the code CMFGEN. The young stellar objects were classified according to their K-band spectra. In combination with published near and mid infrared photometry, we constrained their nature. Linemaps were constructed to study the geometry of their close environment. Results. We identify the ionizing stars of each region. RCW 79 is dominated by a cluster of a dozen O stars, identified for the first time by our observations. RCW 82 and RCW 120 are ionized by two and one O star, respectively. All ionizing stars are early-to-late O stars, close to the main sequence. The cluster ionizing RCW 79 formed 2.3 ± 0.5 Myr ago. Similar ages are estimated, albeit with a larger uncertainty, for the ionizing stars of the other two regions. The total mass-loss rate and ionizing flux is derived for each region. In RCW 79, where the richest cluster of ionizing stars is found, the mechanical wind luminosity represents only 0.1% of the ionizing luminosity, questioning the influence of stellar winds on the dynamics of these three H ii regions. The young stellar objects show four main types of spectral features: H 2 emission, Brγ emission, CO bandheads emission, and CO bandheads absorption. These features are typical of young stellar objects surrounded by disks and/or envelopes, confirming that star formation is taking place on the borders of the three H ii regions. The radial velocities of most YSOs are consistent with that of the ionized gas, firmly establishing their association with the H ii regions. Exceptions are found in RCW 120 where differences up to 50 km s −1 are observed. Outflows are detected in a few YSOs. All YSOs have moderate-to-strong near-IR excess. In the [24] versus K-[24] diagram, the majority of the sources dominated by H 2 emission lines stand out as redder and brighter than the rest of the YSOs. The quantitative analysis of their spectra indicates that, for most of them, the H 2 emission is essentially thermal and likely produced by shocks. We tentatively propose that they represent an earlier phase of evolution compared to sources dominated by Brγ and CO bandheads. We suggest that they still possess a dense envelope in which jets or winds create shocks. The other YSOs have partly lost their envelopes and show signatures of accretion disks. Overall, the YSOs show distinct spectroscopic signatures compared to the ionizing sources, confirming the presence of two stellar populations.

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V1647 Orionis: Reinvigorated Accretion and the Re-Appearance of McNeil's Nebula

Cited by 42 publications

References 29 publications

Photometric and spectroscopic variability of the FUor star V582 Aurigae

Photometric and spectroscopic variability of the FUor star V582 Aurigae

V1647 Orionis: Optical Photometric and Spectroscopic Monitoring Through the 2003-2006 Outburst

Near-IR integral field spectroscopy of ionizing stars and young stellar objects on the borders of H II regions

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