The molecular composition of Comet C/2007 W1 (Boattini): Evidence of a peculiar outgassing and a rich chemistry

Villanueva, G. L.; Mumma, M. J.; DiSanti, M. A.; Bonev, B. P.; Gibb, E. L.; Magee-Sauer, K.; Blake, Geoffrey A.; Salyk, Colette

doi:10.1016/j.icarus.2011.08.024

Cited by 84 publications

(85 citation statements)

References 47 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…These emissions are multiplied by the terrestrial transmittance function; to obtain actual emitted intensities requires dividing by the monochromatic atmospheric transmittance at each Doppler-shifted line position, as discussed in the literature (e.g., see Dello Russo et al 1998;DiSanti et al 2001;Villanueva et al 2011).…”

Section: Discussionmentioning

confidence: 99%

“…We calculated "nucleus-centered" production rates (Q nc ) using our well-established formalism (e.g., see Bonev 2005;Villanueva et al 2011, andSection3.2 of DiSanti et al 2014 for additional details). These are established for each measured line and are based on its flux F line (W m −2 , corrected for telluric transmittance), the molecular photodissociation lifetime (τ 1 , s), and line g-factor (g 1 , W molecule −1 ) at the measured (or adopted) value of T rot (both τ 1 and g 1 correspond to values at…”

Section: Production Ratesmentioning

confidence: 99%

“…In some comets the spatial distribution of HCN suggested the presence of (at least) two phases of ice within the nucleus, one dominated by polar and the other by apolar bonds Villanueva et al 2011Villanueva et al , 2012bPaganini et al 2012;DiSanti et al 2014). In Comet ISON, no clear distinction between profiles of polar and apolar molecules was apparent.…”

Section: Gasmentioning

confidence: 99%

“…This involves applying a correction factor (a "growth factor"; GF in Table 2) established from measured spatial profiles of emission lines, such that Q tot =Q nc ×GF. Our methodology is well documented in the literature; e.g., see Section 3.2 of DiSanti et al (2014), Villanueva et al (2011), Appendix B2 in Bonev et al (2006), and Dello Russo et al (1998) for detailed discussions of the "Q-curve" formalism.…”

Section: A3 Using Spatial Profiles Of Emission To Determine Global mentioning

confidence: 99%

See 3 more Smart Citations

En Route to Destruction: The Evolution in Composition of Ices in Comet D/2012 S1 (Ison) Between 1.2 and 0.34 Au From the Sun as Revealed at Infrared Wavelengths*

DiSanti

Bonev

Gibb

et al. 2016

ApJ

View full text Add to dashboard Cite

We report production rates for H 2 O and eight trace molecules (CO, C 2 H 6 , CH 4 , CH 3 OH, NH 3 , H 2 CO, HCN, C 2 H 2 ) in the dynamically new, Sun-grazing Comet C/2012 S1 (ISON), using high-resolution spectroscopy at Keck II and the NASA IRTF on 10pre-perihelion dates encompassing heliocentric distances R h =1.21-0.34 AU. Measured water production rates spanned two orders of magnitude, consistent with a long-term heliocentric power law) . Abundance ratios for CO, C 2 H 6 , and CH 4 with respect to H 2 O remained constant with R h and below their corresponding mean values measured among a dominant sample of Oort Cloud comets. CH 3 OH was also depleted for R h > 0.5 AU, but was closer to its mean value for R h ≤0.5 AU. The remaining four molecules exhibited higher abundance ratios within 0.5 AU: for R h > 0.8 AU, NH 3 and C 2 H 2 were consistent with their mean values while H 2 CO and HCN were depleted. For R h < 0.5 AU, all four were enriched, with NH 3 , H 2 CO, and HCN increasing most. Spatial profiles of gas emission in ISON consistently peaked sunward of the dust continuum, which was asymmetric antisunward and remained singly peaked for all observations. NH 3 within 0.5 AU showed a broad spatial distribution, possibly indicating its release in the coma provided thatoptical depth effects were unimportant. The column abundance ratio NH 2 /H 2 O at 0.83 AU was close to the "typical" NH/OH from optical wavelengths, but was higher within 0.5 AU. Establishing its production rate and testing its parentage (e.g., NH 3 ) requiremodeling of coma outflow.

show abstract

Section: Discussionmentioning

confidence: 99%

Section: Production Ratesmentioning

confidence: 99%

Section: Gasmentioning

confidence: 99%

Section: A3 Using Spatial Profiles Of Emission To Determine Global mentioning

confidence: 99%

See 2 more Smart Citations

En Route to Destruction: The Evolution in Composition of Ices in Comet D/2012 S1 (Ison) Between 1.2 and 0.34 Au From the Sun as Revealed at Infrared Wavelengths*

DiSanti

Bonev

Gibb

et al. 2016

ApJ

View full text Add to dashboard Cite

show abstract

“…These infrared studies are suggestive of a significant increase in H 2 CO/H 2 O between R h = 0.83 and 0.46 AU. The ratio of H 2 CO/ CH 3 OH in ISON on November 19 (H 2 CO/CH 3 OH = 0.9 ± 0.3) is one of the highest measured in a comet given that H 2 CO/CH 3 OH ranges from $0.01 to 1 over the population measured to date at infrared wavelengths (Bockelée-Morvan et al, 2005;Bonev et al, 2008bBonev et al, , 2009Dello Russo et al, 2004, 2009a, 2014DiSanti et al, 2002DiSanti et al, , 2006DiSanti et al, , 2014Gibb et al, 2012;Mumma et al, 2001bMumma et al, , 2005Mumma and Charnley, 2011;Paganini et al, 2012Paganini et al, , 2014Paganini et al, , 2015Radeva et al, 2010Radeva et al, , 2013Villanueva et al, 2011b). The strong H 2 CO emissions in ISON were sufficient to determine the spatial distribution along the slit on November 19 (Fig.…”

Section: H 2 Comentioning

confidence: 99%

The compositional evolution of C/2012 S1 (ISON) from ground-based high-resolution infrared spectroscopy as part of a worldwide observing campaign

Russo

Vervack

Kawakita

et al. 2016

Icarus

Self Cite

View full text Add to dashboard Cite

The Composition of the Protosolar Disk and the Formation Conditions for Comets

Willacy¹,

Alexander²,

Ali-Dib³

et al. 2017

Comets as Tracers of Solar System Formation and Evolution

View full text Add to dashboard Cite

Conditions in the protosolar nebula have left their mark in the composition of cometary volatiles, thought to be some of the most pristine material in the solar system. Cometary compositions represent the end point of processing that began in the parent molecular cloud core and continued through the collapse of that core to form the protosun and the solar nebula, and finally during the evolution of the solar nebula itself as the cometary bodies were accreting. Disentangling the effects of the various epochs on the final composition of a comet is complicated. But comets are not the only source of information about the solar nebula. Protostellar disks around young stars similar to the protosun provide a way of investigating the evolution of disks similar to the solar nebula while they are in the process of evolving to form their own solar systems. In this way we can learn about the physical and chemical conditions under which comets formed, and about the types of dynamical processing that shaped the solar system we see today.This paper summarizes some recent contributions to our understanding of both cometary volatiles and the composition, structure and evolution of protostellar disks.

show abstract

The molecular composition of Comet C/2007 W1 (Boattini): Evidence of a peculiar outgassing and a rich chemistry

Cited by 84 publications

References 47 publications

En Route to Destruction: The Evolution in Composition of Ices in Comet D/2012 S1 (Ison) Between 1.2 and 0.34 Au From the Sun as Revealed at Infrared Wavelengths*

En Route to Destruction: The Evolution in Composition of Ices in Comet D/2012 S1 (Ison) Between 1.2 and 0.34 Au From the Sun as Revealed at Infrared Wavelengths*

The compositional evolution of C/2012 S1 (ISON) from ground-based high-resolution infrared spectroscopy as part of a worldwide observing campaign

The Composition of the Protosolar Disk and the Formation Conditions for Comets

Contact Info

Product

Resources

About