Meteor Ablated Phosphorus as a Source of Bioavailable P to the Terrestrial Planets
Authors: Douglas Kevin , Mangan Thomas , Carrillo-Sanchez Jaun Diego , Bones David , Feng Wuhu , Blitz Mark , Plane John 
Published: March 2020

&lt;p&gt;&amp;#160; &amp;#160;&amp;#160;&amp;#160;&amp;#160;&amp;#160;&amp;#160;&amp;#160;&amp;#160;&amp;#160;&amp;#160; Phosphorus, P, is a key biological element with major roles in replication, information transfer, and metabolism. Interplanetary dust particles (IDPs) contain ~0.8 % P by elemental abundance, and meteoric ablation in a planetary atmosphere is a significant source of atomic P. Orthophosphate (oxidation state +5) is the dominant form of inorganic P at the Earth&amp;#8217;s surface, however, due to their low water solubility and reactivity, such P(V) salts have a poor bio-availability. Less oxidised forms of P (oxidation state &amp;#8804; +3) are however far more bio-available. Previous studies have focused on the direct delivery of P to the surface in meteorites. In contrast, the atmospheric chemistry of P has so far been ignored.&lt;/p&gt;&lt;p&gt;&amp;#160; &amp;#160; &amp;#160;&amp;#160; &amp;#160;&amp;#160;&amp;#160;&amp;#160; The vaporized P atoms entering the upper atmospheres of the terrestrial planets will undergo chemical processing to form a variety of compounds in which P may exist in different oxidation states due to the presence of both oxidizing and reducing agents. Initial oxidation of P will proceed to produce PO&lt;sub&gt;2&lt;/sub&gt;. From PO&lt;sub&gt;2&lt;/sub&gt;, an exothermic route to phosphoric acid (H&lt;sub&gt;3&lt;/sub&gt;PO&lt;sub&gt;4&lt;/sub&gt;) exists via the formation of HOPO&lt;sub&gt;2&lt;/sub&gt;; however, the bio-available compound phosphonic acid (H&lt;sub&gt;3&lt;/sub&gt;PO&lt;sub&gt;3&lt;/sub&gt;) should also form via HPO&lt;sub&gt;2&lt;/sub&gt;.&lt;/p&gt;&lt;p&gt;&amp;#160;&amp;#160;&amp;#160;&amp;#160;&amp;#160;&amp;#160;&amp;#160;&amp;#160;&amp;#160;&amp;#160;&amp;#160; Using a combination of both experiment and theory, rate coefficients for the reactions of meteor ablated P have been determined. Using a pulsed laser photolysis-laser induced fluorescence (LIF) technique, the reactions of P, PO, and PO&lt;sub&gt;2&lt;/sub&gt; with atmospherically relevant species have been studied as a function of temperature for the first time. Rate coefficients for the subsequent reactions of PO&lt;sub&gt;2&lt;/sub&gt; leading onto to phosphoric and phosphonic acid were calculated from high-level electronic structure calculations.&lt;/p&gt;&lt;p&gt;&amp;#160;&amp;#160;&amp;#160;&amp;#160;&amp;#160;&amp;#160;&amp;#160;&amp;#160;&amp;#160;&amp;#160;&amp;#160; In addition to understanding the reaction kinetics, the delivery of P to the upper atmospheres of Earth, Mars, and Venus via the ablation of IDPs has also been investigated. Using a meteor ablation simulator, micron-size particles were flash heated, and the ablation of PO and Ca recorded simultaneously by LIF. These ablation profiles were used to validate the output of a Chemical Ablation Model (CABMOD), a thermodynamic model that predicts the ablation rates of different elements from IDPs. By combining CABMOD with an astronomical model of dust sources, the global injection rates of P into the atmospheres of Earth, Mars, and Venus has been estimated to be 0.017, 1.15&amp;#215;10&lt;sup&gt;-3&lt;/sup&gt;, and 0.024 t d&lt;sup&gt;-1&lt;/sup&gt; (tonnes per Earth day) respectively.&lt;/p&gt;&lt;p&gt;&amp;#160;&amp;#160;&amp;#160;&amp;#160;&amp;#160;&amp;#160;&amp;#160;&amp;#160;&amp;#160;&amp;#160;&amp;#160; The results from the kinetics experiments, together with the P injection rates from CABMOD, have been input into a global chemistry-climate model of the Earth&amp;#8217;s atmosphere (WACCM). Using WACCM, the relative amounts of phosphoric and phosphonic acid produced from meteor ablated P in the Earth&amp;#8217;s atmosphere can be assessed. Preliminary results indicated that both H&lt;sub&gt;3&lt;/sub&gt;PO&lt;sub&gt;4&lt;/sub&gt;, and the bio-available H&lt;sub&gt;3&lt;/sub&gt;PO&lt;sub&gt;3&lt;/sub&gt; are formed, with around a third of the ablated P ending up as H&lt;sub&gt;3&lt;/sub&gt;PO&lt;sub&gt;3&lt;/sub&gt;. Further work is also underway to determine where on the Earth&amp;#8217;s surface H&lt;sub&gt;3&lt;/sub&gt;PO&lt;sub&gt;3&lt;/sub&gt; will be deposited, to understand how accretion rates would have differed on the early Earth, and to input the P chemical scheme into a Mars atmospheric model.&lt;/p&gt;